research annual report 2012 · 2019. 9. 16. · zhangyin zhao, jin chan, sheng-cai shi, yuehua ma,...

Research Annual Report

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科

研

工

作

年

度

报

告

2012

中国科学院紫金山天文台

2012 科研工作年度报告

中国科学院紫金山天文台科技处

2013 年 9 月

Cover: A sample NST He I 10830 Å narrow band filtergram (see Page 97 for details)

封面：最高分辨率的氦 1083 纳米谱线色球像 (详见第 97 页)

Annual Report’2012－Content

I

目录

2012 年度科研工作总结 ........................................................................................ 1

2012 年度发表论文摘要 (Abstract List Of Publications In 2012) .................. 19

I. Dark Matter & Space Astronomy .............................................................. 20

Cosmology, Dark Matter and High-Energy Astrophysics ................................ 20

(1) Scientific Achievements of Prof. Chien Shiung Wu, Asia Pac. Phys. Newslett,

1, 2, Lu, Tan* ................................................................................................. 20

(2) Constraining Dark Energy Using Observational Growth Rate Data, PHYSICS

LETTERS B, 717, Lu, Tan ............................................................................ 20

(3) A Comprehensive Comparison of Cosmological Models from the Latest

Observational Data, MNRAS, 426, 3, Lu, Tan .............................................. 20

(4) Toward Tight Gamma-Ray Burst Luminosity Relations, APJ, 749, 2, Qi, Shi*

20

Gamma-Ray Burst, Neutron Star and relevant physics ................................... 21

(5) Discrete Mass Ejections from the Be/X-Ray Binary A0535+26/HD 245770,

APJ, 744, 1, Yan, Jingzhi*.............................................................................. 21

(6) Revisiting the Long/Soft-Short/Hard Classification of Gamma-Ray Bursts In

the Fermi Era, APJ, 750, 2, Zhang, Fu-Wen* ................................................. 21

(7) Gamma-Ray Bursts: The Isotropic-Equivalent-Energy Function and the

Cosmic Formation Rate, MNRAS,423, 3, Wu, Shi-Wei* ............................... 21

(8) Multi-Wavelength Study Of the Be/X-Ray Binary MXB 0656-072, APJ, 753,

1, Yan, Jingzhi* .............................................................................................. 21

(9) X-Ray and Optical Observations of A 0535+26, APJ, 754, 1, Yan, J. ........... 22

(10) Gamma-Ray Bursts and Other Observations: Constraints on Cosmographic

Parameters and Dark Energy Models, CAA, 36, 2, Liu, Jian-wei* ............... 22

(11) Analytical Afterglow Light Curves of Gamma-ray Bursts: the Case of a Flat

Electron Spectrum, CAA, 36, 2, Wang, Y.* .................................................... 22

(12) Early Afterglow Emission as a Probe of the Density Profile of the Medium

Surrounding Gamma-Ray Bursts, MSAIS, 21, Jin, Z. P.* ............................. 22

High-Energy Solar Astrophysics ........................................................................ 23 (13) On the Frequency Distributions of Solar Soft X-ray Flares, EAS Publications

Series, 55, Gan, W. Q.* .................................................................................. 23

(14) China’s Space Astronomy and Solar Physics in 2011-2012, Chin J Space Sci,

32, 5, GAN, Weiqun ....................................................................................... 23

(15) The Calculation of Solar Gamma-Rays by TALYS, CAA, 36, 1, Chen, Wei* 23

(16) Ground-Based giant solar Telescope of China, SSPMA, 42, 12, Ji, haisheng

23

(17) Commission 12: Solar Radiation and Structure, SSPMA, 7, T28A, Alexander

Kosovichev* ................................................................................................... 23

(18) An Observational Study on Coronal Hard X-ray Sources in Flares, CAA, 36,

3, Bai, Wei-dong* ........................................................................................... 24

(19) An Attempt at a Unified Model for the Gamma-Ray Emission of Supernova

Remnants, APJ, 761, 2, Yuan, Qiang* ........................................................... 24

(20) Solar Flares with an Exponential Growth of the Emission Measure in the

Impulsive Phase Derived from X-ray Observations, AcASn, 53, 6, HAN,

Fei-ran* ......................................................................................................... 24

(21) Statistical Study of Emerging Flux Regions and the Response of the Upper

Atmosphere, RIAA, 12, 12, Zhao, Jie*.......................................................... 24

(22) The Past and Future of Space Solar Observations, SSPMA, 42, 12, GAN,

WeiQun* ......................................................................................................... 25

(23) The effect of Compton scattering on gamma-ray spectra of the 2005 January

20 flare, RIAA, 12, 10, Chen, Wei* ............................................................... 25

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第一作者文章。

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II

(24) An Interpretation of the Possible Mechanisms of Two Ground-Level

Enhancement Events, APJ, 758, 2, Firoz, Kazi A.* ........................................ 25

(25) Improvements to the X-ray Bremsstrahlung Thick-target Model and Their

Applications to Solar Flare Observations, AcASn, 53, 2, Su, Yang*.............. 26

(26) Particle kinetic analysis of a polar jet from SECCHI COR data, AA, 538,

Feng, L.* ....................................................................................................... 26

(27) Evolution of Hard X-Ray Sources and Ultraviolet Solar Flare Ribbons for a

Confined Eruption of a Magnetic Flux Rope, APJ, 746, 1, Li, H. ................. 26

(28) Statistical Analyses on Thermal Aspects of Solar Flares, APJ, 747, 2,

Li, Y. P.* ......................................................................................................... 26

(29) Morphological Evolution of a Three-Dimensional Coronal Mass Ejection

Cloud Reconstructed From Three Viewpoints, APJ, 751, 1, Feng, L.*.......... 27

(30) Solar Intranetwork Magnetic Elements: Bipolar Flux Appearance, SOLAR

PHYSICS, 278, 2, Li, Hui ............................................................................. 27

(31) A Teardrop-Shaped Ionosphere At Venus In Tenuous Solar Wind, PSS, 73, 1,

Feng, L. ......................................................................................................... 27

(32) Unusual Emissions at Various Energies Prior to the Impulsive Phase of the

Large Solar Flare and Coronal Mass Ejection of 4 November 2003, SOLAR

PHYSICS, 279, 2, Su, Yang ........................................................................... 28

(33) Solar Magnetized "Tornadoes:" Relation to Filaments, APJL, 756, 2, Su,

Yang* ............................................................................................................. 28

(34) Particle Acceleration and Gamma Rays in Solar Flares: Recent Observations

and New Modeling, ASR, 50, 6, Gan, W. Q. ................................................. 28

Multi-Band Observation of Solar Activity ......................................................... 29 (35) Slowly Drifting Radio Structures in Solar Flares, Astronomical Research &

Technology, 9, 4, Ning, Zongjun* .................................................................. 29

(36) The Contraction and Shearing of Solar Flare Loops, Astronomical Research

& Technology, 9, 4, Zhou, Tuanhui* .............................................................. 29

(37) Radiative and Conductive Cooling In a Solar Flare, ASS, 338, 1, Ning,

Zongjun* ........................................................................................................ 29

(38) Magnetic Bright Points in the Solar Atmosphere, Progress in Astronomy, 30,

2, Li, Dong* ................................................................................................... 29

(39) Power Conversion Factor in Sollar Flares, CHINESE SCIENCE BULLETIN,

57, 12, Ning, ZongJun* .................................................................................. 30

(40) Observation of Ultrafine Channels of Solar Corona Heating, APJL, 570, 1, Ji,

Haisheng* ...................................................................................................... 30

(41) Frequency Dependence of the Power-Law Index of Solar Radio Bursts, APJ,

570, 2, Song, Qiwu* ....................................................................................... 30

(42) UV1600 Bright Points and Magnetic Bipoles in Solar Quiet Regions, ASS,

341, 2, Li, Dong* ........................................................................................... 30

Laboratory for Dark Matter and Space Astronomy ......................................... 31 (43) GRB 120422A: A Low-Luminosity Gamma-Ray Burst Driven By a Central

Engine, APJ, 756, 2, Fan, Yi-Zhong .............................................................. 31

(44) Statistical Interpretation of the Spatial Distribution of Current 130 GeV

Gamma-Ray Line Signal Within the Dark Matter Annihilation Scenario,

PHYSICS LETTERS B, 756, 4-5, Yang, Rui-Zhi* ........................................ 31

(45) The Photospheric Radiation Model for the Prompt Emission of Gamma-Ray

Bursts: Interpreting Four Observed Correlations, APJL, 755, 1, Fan,

Yi-Zhong* ....................................................................................................... 31

(46) Fermi Large Area Telescope Observations of GRB 110625A, APJ, 754, 2,

Fan, Yi-Zhong ................................................................................................ 32

(47) Deep observation of the giant radio lobes of Centaurus A with the Fermi

Large Area Telescope, APJL, 755, 1, Fan, Yi-Zhong* ................................... 32

(48) Estimating The Background Count Rate in the Energy Field From 0.55-2.75

MeV for Chang'E-1 Gamma-Ray Spectrometer, NUCLEAR INSTRUMENTS

PMO

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Editor Commettee

Darun XIONG, Tan LU

Ji YANG, Chunlin LU, Weiqun GAN

Zhangyin ZHAO, Jin CHAN,

Sheng-Cai SHI, Yuehua MA,

Daming WEI, Haisheng JI,

Longlong FENG, Xi KANG, Yu GAO,

Hongchi WANG, Ye XU, Jin Xu,

Dazhi YAO, Yanning FU, Weibiao XU

Jianghui JI, Haibin ZHAO

Sub-Editor

Liubing ZHU [email protected]

Excutive Editor

Rui-Qing MAO [email protected]

Division of

Science & Technology Management


http://www.pmo.cas.cn/




III

& METHODS IN PHYSICS RESEARCH SECTION A, 664, 1, Ma, T.* .... 32

(49) GRB 081029: A Gamma-Ray Burst with A Multi-Component Afterglow, APJ, 745, 1, Fan, Yi-Zhong .... 32

(50) Dark Matter Mini-Halo around the Compact Objects: The Formation, Evolution and Possible Contribution

to the Cosmic Ray Electrons/Positrons, JOCAP, 2012, 01, Yang, Rui-Zhi* ........................................................ 33

(51) A High Dynamic Range Readout Unit for a Calorimeter, CHINESE PHYSICS C, 36, 1, Guo Jian-Hua 33

(52) CHANDRA/HETGS Observations of the Brightest Flare Seen From Sgr A*, APJ, 759, 2, Ji, L. ............ 33

(53) Readout Electronics Design of prototype of BGO Calorimeter in Chinese Space Detector for Dark Matter

Particle, AcASn, 53, 1, Guo, Jianhua*................................................................................................................ 33

(54) Development of the DAQ System of Chinese High Energy Cosmic Ray Detector in Space, 32nd

international cosmic ray conference, 5, Guo jianhua* ........................................................................................ 33

(55) Expected Performance of the Chinese High Energy Cosmic Particle Detector to Be In Space, 32nd

international cosmic ray conference, 5, Wu, J.* .................................................................................................. 34

(56) Study of Backward-Propagating Langmuir Waves with Numerical Simulations Based on the

Particle-in-Cell Method, Astronomical Research & Technology, 9, 4, Huang, Yu* ............................................ 34

(57) Ejected-Electron Spectroscopy of Autoionizing Resonances of Helium Excited By Fast-Electron Impact,

Physical Review A, 86, 6, Zhang, Zhe* .............................................................................................................. 34

(58) Mechanical Design of BGO Calorimeter for Chinese High Energy Cosmic Ray Detector in Space, 32nd

international cosmic ray conference, 5, Yiming, Hu* .......................................................................................... 34

II. Antarctic Astronomy Radio Astronomy .............................................................................................. 35

Stellar Structure, Evolution and Pulsation ..................................................................................................... 35 (59) Sound-Speed Inversion of the Sun Using a Nonlocal Statistical Convection Theory, APJL, 759, 1, Xiong,

Darun.................................................................................................................................................................. 35

Center for Antarctic Astronomy ...................................................................................................................... 35 (60) Status of the First Antarctic Survey Telescopes for Dome A, Proceedings of SPIE, 8444, 1, Wang, Lifan 35

(61) Operation, Control, and Data System for Antarctic Survey Telescope (AST3), Proceedings of the SPIE,

8448, Wang, Lifan ............................................................................................................................................... 35

(62) Bulk Flow of Halos in Lambda CDM Simulation, APJ, 761, 2, Li, Ming* ................................................ 36

(63) The Dynamical State and Mass-Concentration Relation of Galaxy Clusters, MNRAS, 427, 2, Li, Ming . 36

(64) Precipitable Water Vapor above Dome A, Antarctica, Determined From Diffuse Optical Sky Spectra,

PASP, 124, 911, Feng, LongLong ....................................................................................................................... 36

(65) Physical Origin of Multi-Wavelength Emission of GRB 100418A and Implications for Its Progenitor,

RIAA, 12, 4, Wu, Xue-Feng ................................................................................................................................ 36

(66) Modeling Photodisintegration-Induced TeV Photon Emission from Low-Luminosity Gamma-Ray Bursts,

AJ, 143, 5, Wu, Xue-Feng ................................................................................................................................... 37

(67) Panchromatic Observations of the Textbook GRB 110205a: Constraining Physical Mechanisms of Prompt

Emission and Afterglow, APJ, 751, 2, Wu, X. F. ................................................................................................. 37

(68) Airglow and Aurorae at Dome A, Antarctica, PASP, 124, 916, Feng, LongLong ...................................... 38

(69) GRB 110721A: Photosphere "Death Line" And the Physical Origin of the GRB Band Function, APJL,

758, 2, Wu, Xue-Feng ......................................................................................................................................... 38

Galaxy Cosmology and Dark Energy.............................................................................................................. 38

(70) Exploring Galaxy Formation Models and Cosmologies with Galaxy Clustering, MNRAS, 422, 1,

Kang, X.* ............................................................................................................................................................. 38

Star Formation in Galaxies ...................................................................................................................... 39

(71) Little Things, AJ, 144, 5, Zhang, Hong-Xin ............................................................................................... 39

(72) Some Updates on the Star Formation Laws in Galaxies, AAS Meeting, 220, 308, Gao, Yu* ..................... 39

(73) High Resolution SMA Imaging of (Ultra)-Luminous Infrared Galaxies, Proceedings IAU Symposium,

284, Tan, Qinghua* ............................................................................................................................................. 39

(74) The Molecular Gas in Luminous Infrared Galaxies - I. CO Lines, Extreme Physical Conditions and Their

Drivers, MNRAS, 426, 4, Gao, Yu...................................................................................................................... 39

(75) The Stellar and Gas Kinematics of the Little Things Dwarf Irregular Galaxy NGC 1569, AJ, 144, 4, Zhang,

Hong-Xin ............................................................................................................................................................ 40

(76) Major-Merger Galaxy Pairs In the Cosmos Field-Mass-Dependent Merger Rate Evolution since z=1, APJ,

747, 2, Zhao, Yinghe ........................................................................................................................................... 40

(77) Stellar Populations of Classical and Pseudo-Bulges for a Sample of Isolated Spiral Galaxies, ASS, 337, 2,

Zhao, Yinghe* ...................................................................................................................................................... 41


IV

(78) Large-Scale Kinematics, Astrochemistry, and Magnetic Field Studies of Massive Star-Forming Regions

through HC3N, HNC, and C2H Mappings, APJ, 745, 1, Zhang, Zhi-yu ............................................................ 41

(79) The Global Star Formation Law of Galaxies Revisited In the Radio Continuum, SCI CHINA PHYS

MECH, 55, 2, Liu, LiJie* .................................................................................................................................... 41

(80) Tidal Dwarf Galaxies at Intermediate Redshifts, ASS, 337, 2, Wen, Zhang-Zheng* .................................. 42

(81) Outside-In Shrinking Of the Star-Forming Disk of Dwarf Irregular Galaxies, AJ, 143, 2, Zhang,

Hong-Xin* ........................................................................................................................................................... 42

(82) In-Spiraling Clumps in Blue Compact Dwarf Galaxies, APJ, 747, 2, Zhang, Hong-Xin ........................... 42

(83) Molecular Gas in Infrared Ultraluminous QSO Hosts, APJ, 750, 2, Gao, Y. ............................................. 43

(84) The Molecular Gas in Luminous Infrared Galaxies. II. Extreme Physical Conditions and Their Effects on

the X-Co Factor, APJ, 751, 1, Gao, Yu................................................................................................................ 43

(85) H I Power Spectra and the Turbulent Interstellar Medium of Dwarf Irregular Galaxies, APJ, 754, 1, Zhang,

Hong-Xin* ........................................................................................................................................................... 43

Molecular Clouds and Star Formation ........................................................................................................... 44 (86) A Herschel Survey of Cold Dust in Disks around Brown Dwarfs and Low-Mass Stars, APJ, 755, 1,

Liu, Yao ............................................................................................................................................................... 44

(87) Different Evolutionary Stages in the Massive Star-Forming Region W3 Main Complex, APJ, 754, 2, Wang,

Yuan* ................................................................................................................................................................... 44

(88) LAMOST Experiment for Galactic Understanding and Exploration (LEGUE) - The Survey's Science Plan,

RIAA, 12, 7, Wang, Hong-Chi............................................................................................................................ 44

(89) An Algorithm for Preferential Selection of Spectroscopic Targets in LEGUE, RIAA, 12, 7, Wang,

Hong-Chi ............................................................................................................................................................ 45

(90) The Site Conditions of the Guo Shou Jing Telescope, RIAA, 12, 7, Wang, Hong-Chi .............................. 45

(91) The LEGUE Input Catalog for Dark Night Observing in the LAMOST Pilot Survey, RIAA, 12, 7, Wang,

Hong-Chi ............................................................................................................................................................ 45

(92) The LEGUE High Latitude Bright Survey Design For the LAMOST Pilot Survey, RIAA, 12, 7, Wang,

Hong-Chi ............................................................................................................................................................ 46

(93) The LEGUE Disk Targets for LAMOST's Pilot Survey, RIAA, 12, 7, Wang, Hong-Chi .......................... 46

(94) A Resonant Feature near The Perseus Arm Revealed by Red Clump Stars, APJL, 753, 1, Fang, Min ...... 46

(95) A Population of Isolated Hard X-Ray Sources near The Supernova Remnant Kes 69, AA, 541, Zhou, X. 46

(96) Star formation and disk properties in Pismis 24, AA, 539, Fang, M.* ....................................................... 47

(97) Unveiling the Physical Properties and Kinematics of Molecular Gas in the Antennae Galaxies (NGC

4038/9) Through High-Resolution CO (J=3-2) Observations, APJ, 745, 1, Mao, Rui-Qing .............................. 47

(98) Age Spread in W3 Main: Large Binocular Telescope/LUCI Near-Infrared Spectroscopy of The Massive

Stellar Content, APJ, 744, 2, Wang, Y. ................................................................................................................ 48

(99) DoAr 33: A Good Candidate for Revealing Dust Growth and Settling In Protoplanetary Disks, AA, 546,

Y. Liu* ................................................................................................................................................................. 48

(100) Type IIn SUPERNOVA SN 2010jl: Optical Observations for Over 500 Days after Explosion, AJ, 144, 5,

Wang, Min ........................................................................................................................................................... 48

(101) Constraints on the Dark Matter Annihilation Scenario of Fermi 130 GeV Gamma-Ray Line Emission by

Continuous Gamma-Rays, Milky Way Halo, Galaxy Clusters and Dwarf, JCAP, 2012, 11, Yuan, Qiang ......... 49

(102) Near-Infrared Imaging Polarization Study of M 17, PASJ, 64, 5, Chen, Zhiwei* .................................... 49

Laboratory for Millimeter & Sub-Millimeter Wave ...................................................................................... 49 (103) Spectral Response and Noise Temperature of a 2.5 THz Spiral Antenna Coupled NbN HEB Mixer,

Physics Procedia, 36, Zhang, W* ........................................................................................................................ 49

(104) Study on the Optics of the 5 Meter Dome A Terahertz Explorer (DATE 5) for Antarctica, ISAPE2012,

Lou, Zheng*......................................................................................................................................................... 50

(105) Temperature-Dependent Performances of Nb SIS Mixers at Millimeter and Submillimeter Wavelength,

ICMMT, 5, Liu, Jie* ............................................................................................................................................ 50

(106) Effects of Multiple Reflections and Low-Frequency Interferences on Measured Terahertz Fourier

Transform Spectra, Proceedings of SPIE, 8562, Li, Shao-Liang* ....................................................................... 50

(107) A Novel Quasi-Optical Subharmonically Pumped GaAs Diode Mixer at 375 GHz, Proceedings of SPIE,

8562, Hu, Jie* ..................................................................................................................................................... 50

(108) Readout System for the Terahertz Superconducting Imaging Array (TeSIA), Proceedings of SPIE, 8562,

Li, Sheng* ............................................................................................................................................................ 51

(109) Atmospheric Profiling Synthetic Observation System at THz, Proceedings of SPIE, 8562, Yao, Qijun* 51

(110) Development of Superconducting Spectroscopic Array Receiver: A Multibeam 2SB SIS Receiver for


V

Millimeter-Wave Radio Astronomy, IEEE Transactions on Terahertz Science and Technology, 2, 6, Shan,

Wenlei* ................................................................................................................................................................ 51

(111) Influence of Substrate on Coupling of High Temperature Superconducting Josephson junction Arrays,

Physica C: Superconductivity, 483, 14, Wang, Zh. ............................................................................................. 51

(112) Development of Superconducting Mixers for THz Astronomy, SCIENCE CHINA-INFORMATION

SCIENCES, 55, 1, Shi, ShengCai*...................................................................................................................... 52

(113) Stabilized Hot Electron Bolometer Heterodyne Receiver at 2.5 THz, APL, 100, 8, Ren, Y. .................... 52

(114) Radiation from Intrinsic Josephson Junctions in Misaligned Tl2Ba2CaCu2O8 Thin Films, J

SUPERCOND NOV MAGN, 25, 5, Wang, Z. .................................................................................................... 52

(115) Terahertz Wavefronts Measured Using the Hartmann Sensor Principle, Optics Express, 20, 13, Ren, Y. 52

(116) Direct Detection of Terahertz Signals at 493GHz Using Nb Superconducting Tunnel Junctions, ICMMT,

2, Wang, Zheng* .................................................................................................................................................. 52

(117) Frequency Locking Of Single-Mode 3.5-THz Quantum Cascade Lasers Using a Gas Cell, APL, 100, 4,

Ren, Y.* ................................................................................................................................................................ 52

(118) Analysis of Multiport Passive Components Using Admittance Matrix, ICMMT, 2, Yang, JinPing ........ 53

(119) Frequency and Amplitude Stabilized Terahertz Quantum Cascade Laser as Local Oscillator, APL, 101,

10, Ren, Y.* .......................................................................................................................................................... 53

(120) Millimeter-Wave Radiation from Misaligned Tl2Ba 2CaCu2O8 Thin-Film Intrinsic Josephson Junctions,

IEEE T APPL SUPERCON, 22, 5, Wang Zh. ..................................................................................................... 53

(121) Twin Slot Antenna Patterns of a Quasi-Optical HEB Mixer at THz Frequencies, ICMMT, 5, Zhou,

K.M.*

................................................................................................................................................................ 53

(122) Research on the Equivalent Circuit of Microstrip T-Junctions and Its Application on Branch-Line

Coupler, ICMMT, 1, Yang, Jin-Ping ................................................................................................................... 53

(123) Temperature-dependent Performances of Nb SIS Mixers at Millimeter and Submillimeter Wavelength

Microwave and Millimeter Wave Technology, ICMMT, 5, Liu, Jie* .................................................................. 54

(124) Development of a 385-500 GHz Sideband-Separating Balanced SIS Mixer, JIRMW, 33, 10, Shan,

Wenlei ............................................................................................................................................................... 54

(125) An Effective Method for Improving Emissions from Intrinsic Josephson Junction Arrays of Misaligned

Tl2Ba2CaCu2O8+delta Thin Films, J SUPERCOND NOV MAGN, 25, 7, Wang, Z.* ...................................... 54

(126) Exact De Sitter Solutions in Quadratic Gravitation with Torsion, CLASSICAL AND QUANTUM

GRAVITY, 29, 23, Chee, Guoying* .................................................................................................................... 54

Qinhai Observation Station ..................................................................................................................... 55 (127) A Sensitive Survey of Dense Parts of Outflows toward Massive Cores, AcASn, 53, 2, Sun, Yan

* .......... 55

(128) Trigonometric Parallaxes of Massive Star-Forming Regions. IX. The Outer Arm in the First Quadrant,

APJ, 745, 1, Xu, Y. .............................................................................................................................................. 55

(129) Massive Star Formation toward G28.87+0.07 (IRAS 18411-0338) Investigated By Means Of Maser

Kinematics and Radio to Infrared Continuum Observations, APJ, 749, 1, Li, J. J.* ........................................... 55

(130) A 95 GHz Class I Methanol Maser Survey toward a Sample of Glimpse Point Sources Associated With

BGPS Clumps, APJS, 200, 1, Xu, Ye .................................................................................................................. 56

(131) Gas Emissions in Planck Cold Dust Clumps-A Survey of the J=1-0 Transitions of (CO)-C-12,

(CO)-C-13, And (CO)-O-18, APJ, 756, 1, Ju, Bing-Gang .................................................................................. 56

(132) Trigonometric Parallax of RCW 122, Proceedings IAU Symposium, 287, Wu, Y. W.* ............................ 56

(133) Massive Star-Formation toward G28.87+0.07, SSA, 749, 1, Li, JJ* ........................................................ 57

(134) Methanol Maser Parallaxes and Proper Motions, Proceedings IAU Symposium, 287, Xu, Y.* ................ 57

III. Applied Celestial Mechanics and Space Object & Debris Research ................................................. 58

Center for Space Object and Debris Research ............................................................................................... 58 (135) Use of Mathematic Morphological Operators for Processing the Smeared Images of a Camera without

Shutter, CAA, 36, 3, Sun, Rong-yu* .................................................................................................................... 58

(136) A New Approach to the Electro-optical Tracking of a Space Object, AcASn, 53, 2, Wang, Xin* ............ 58

(137) Assignment of Space Objects for Electro-Optical Observation Network, Journal of Spacecraft TT&C

Technology, 31, 6, Wang, Xin* ............................................................................................................................ 58

(138) A Definite Integration Method of Calculating Inclination Function and its Derivative, AcASn, 53, 1, Wu,

Lianda* ............................................................................................................................................................... 58

(139) An Automatic Identification Method for GEO Space Objects, Journal of Spacecraft TT&C Technology,

31, 6, Sun, Rongyu* ............................................................................................................................................. 58

(140) Optical Survey Technique for Space Debris in GEO, Progress in Astronomy, 30, 3, Sun, Rongyu* ........ 59

(141) Two Methods for Deriving the Recursion Formula of Inclination Function, AcASn, 53, 5, Wu, Lianda* 59


VI

(142) A New Approach to the Electro-optical Tracking of a Space Object, AcASn, 53, 2, Wang, Xin* ............ 59

(143) On The Triangular Libration Points in Photogravitational Restricted Three-Body Problem with Variable

Mass, ASS, 337, 1, Zhang, Ming-Jiang* ............................................................................................................. 59

(144) Using Operators of Morphological Mathematic for Processing Smeared Image of Camera without

Shutter, AcASn, 53, 1, Sun, Rongyu* .................................................................................................................. 60

(145) A Definite Integration Method of Calculating Inclination Function and its Derivative, AcASn, 53, 1, Wu,

Lianda* ............................................................................................................................................................... 60

(146) A New Method for Detecting GEO Space Objects with Image Stacking, AcASn, 53, 3, Sun, Rongyu* . 60

(147) Low-thrust Trajectory Optimization Using Indirect Shooting Method without Initial Costate Guess,

AcASn, 53, 3, Lin, Houyuan* ............................................................................................................................. 60

(148) Mei Symmetry of Discrete Mechanico-Electrical Systems, ACTA MECH, 223, 4, Zhang, M. J.* .......... 60

(149) Perturbation to Noether Symmetry and Noether Adiabatic Invariants of Discrete Difference Variational

Hamilton Systems, ACTA PHYSICA POLONICA A, 122, 1, Zhang, M. -J.* .................................................... 61

(150) Reply To: "Comment On The Paper 'On The Triangular Libration Points In Photogravitational Restricted

Three-Body Problem With Variable Mass'" By Varvoglis, H. and Hadjidemetriou, J.D., APSS, 340, 2, Zhang,

Ming-Jiang* ........................................................................................................................................................ 61

(151) A Method of Separating Blended Images in Space Debris Observation, SCPMA, 55, 10, Sun, RongYu* 61

Laboratory for CCD Camera Development ................................................................................................... 61 (152) A High Speed Data Transmission System Based on Optic Fiber and PCI Bus, Optical Communication

Technology, 36, 5, Kou Chaoyong* .................................................................................................................... 61

(153) Design of CCD Camera Based on Gigabit Ethernet, LOP, 49, 3, Men Jinrui* ........................................ 61

(154) The ROI Image Abstraction Technology of 1 k×1 k CCD Camera, OPTOELECTRONIC

TECHNOLOGY, 32, 2, Liu, Wei* ....................................................................................................................... 62

Precise Orbit Determination of Spacecraft .................................................................................................... 62 (155) Application of Numerical Integration and Data Fusion in Unit Vector Method, AcASn, 53, 1, Zhang,

Jing*

................................................................................................................................................................ 62

(156) The Study and Applications of Satellite and Satellite Constellation Autonomous Orbit Determination

Using Star Sensor, AcASn, 53, 4, Gan, Qingbo* ................................................................................................ 62

IV. Planetary Sciences and Deep Space Exploration ................................................................................ 62

Near Earth Object Survey and Solar System Bodies ..................................................................................... 62 (157) Activity of Comet 103P/Hartley 2 from September 30 to November 04, 2010, SCPMA, 55, 8, Shi,

JianChun* ........................................................................................................................................................... 62

(158) Numerical Simulation of Time Delay Interferometry for a LISA-like Mission with the Simplification of

Having Only One Interferometer, ASR, 51, 1, Wang, Gang ............................................................................... 62

(159) Astrodynamical Space Test of Relativity Using Optical Devices I (ASTROD I)-a Class-M Fundamental

Physics Mission Proposal for Cosmic Vision 2015-2025: 2010 Update, EXPERIMENTAL ASTRONOMY, 34,

2, Wang, Gang .................................................................................................................................................... 63

Ephemerial Astronomy and Astronomical Reference System ...................................................................... 63 (160) Binary Orbit Determination by Using a Variety of Observational Data, AcASn, 53, 3, Ren Shulin

*....... 63

(161) The Transformation between Tau and TCB for Deep Space Missions under IAU Resolutions, RIAA, 12,

6, Deng, Xue-Mei* .............................................................................................................................................. 64

(162) Two-post-Newtonian Light Propagation in The Scalar-Tensor Theory: An N-Point Mass Case,

PHYSICAL REVIEW D, 86, 4, Deng, Xue-Mei* .............................................................................................. 64

The Sun and Solar System Plasmas ................................................................................................................ 64 (163) The Nonlinear Wave-Wave Interaction of the Kinetic Alfvdn Wave and Its Application in the

Solar-Terrestrial Space Plasmas, AcASn, 53, 5, ZHAO, Jin-song* ..................................................................... 64

(164) Electron Cyclotron Maser Instability in Space Plasmas with Kappa Loss-Cone Distribution, APJ, 745, 2,

Tang, J. F.* .......................................................................................................................................................... 64

(165) Alfvenic Turbulence Generated By a Beam of Energetic Ions via Spontaneous Process, PHYSICS OF

PLASMAS, 19, 2, Wu, D. J.* .............................................................................................................................. 65

(166) Effects of Power-Law Spectrum Behaviors of Nonthermal Electrons on a Ring-Beam Maser Instability,

SCPMA, 55, 4, Tang, JianFei* ........................................................................................................................... 65

(167) Euler Potentials' Discontinuity In The Presence Of Field Line-Aligned Currents, CHINESE SCIENCE

BULLETIN, 57, 12, Huang, TianSen* ................................................................................................................ 65

(168) The Evidence for the Evolution of Interplanetary Small Flux Ropes: Boundary Layers, CHINESE

SCIENCE BULLETIN, 57, 12, Wu DeJin.......................................................................................................... 65


VII

(169) On Theories of Solar Type III Radio Bursts, CHINESE SCIENCE BULLETIN, 57, 12, Wu,

ChingSheng* ....................................................................................................................................................... 66

(170) Basic Plasma Processes in Solar-Terrestrial Activities, , CHINESE SCIENCE BULLETIN, 57, 12, Wu

DeJin*

................................................................................................................................................................ 66

(171) Convective Cell Generation by Kinetic Alfven Wave Turbulence in the Auroral Ionosphere, PHYSICS

OF PLASMAS, 19, 6, Zhao, J. S.* ..................................................................................................................... 66

(172) Kinetic Alfven Wave Instability Driven By Field-Aligned Currents in Solar Coronal Loops, APJ, 754, 2,

Chen, L.* ............................................................................................................................................................. 66

(173) Dispersion Equation of Low-Frequency Waves Driven by Temperature Anisotropy, PST, 14, 10, Chen,

L.*

................................................................................................................................................................. 67

(174) Resonant Wave-Particle Interactions Modified By Intrinsic Alfvenic Turbulence, PHYSICS OF

PLASMAS, 19, 8, Wu, D. J. ............................................................................................................................... 67

Laboratory for Astrochemistry and Planetary Sciences ............................................................................... 67 (175) Water Content, Chlorine and Hydrogen Isotope Compositions of Lunar Apatite., MPS, 47, Wang, Y.

* .. 67

(176) Petrology and Mineralogy of the Tissint Olivine-Phyric Shergottite, MPS, 47, Hsu, Weibiao* ............... 67

(177) Oxygen Isotopes of Al-Rich Chondrules from Unequilibrated Ordinary Chondrites, MPS, 47, Hsu, W.*67

(178) Petrogenesis of the Northwest Africa 4734 basaltic lunar meteorite, GCA, 92, Wang, Ying* .................. 68

(179) Petrogenesis of Grove Mountains 020090: An Enriched "Lherzolitic" Shergottite, MPS, 47, 9, Jiang,

Yun*

................................................................................................................................................................. 68

Xuyi Observation Station ..................................................................................................................... 68 (180) Distribution of PSF of Near Earth Object Survey Telescope, AcASn, 53, 3, Li, Bin

*.............................. 68

(181) The 2009 Apparition of Methuselah Comet 107P/Wilson-Harrington: A Case of Comet Rejuvenation?,

PSS, 70, 1, Zhao, H. ........................................................................................................................................... 69

Laboratory for Planetary Science and Deep Space Exploration .................................................................. 69 (182) The ASTROD I Charging Simulation and Disturbances Due To Solar Energetic Particles at 0.5 AU,

ACTA ASTRONAUTICA, 77, Bao, Gang* ........................................................................................................ 69

(183) Predicting the Configuration of a Planetary System: KOI-152 Observed By Kepler, APJ, 753, 2, Wang,

Su*

................................................................................................................................................................ 70

(184) Tidal Evolution of Exo-Planetary Systems: WASP-50, GJ 1214 and CoRoT-7, SCPMA, 55, 5, Dong,

Yao*

................................................................................................................................................................. 70

(185) The Simulation of Radiation Effects to Astronauts Due To Solar Energetic Particles in Deep Space,

ACTA ASTRONAUTICA, 71, 5, Bao, Gang* .................................................................................................... 70

(186) The Internal Structure Models of Europa, ACTA ASTRONAUTICA, 55, 1, Jin, Sheng* ....................... 70

(187) Possible Origin of the Damocloids: The Scattered Disk or a New Region?, RIAA, 12, 11, Wang, Su*... 71

(188) Grain Growth in Protoplanetary Disks, Progress in Astronomy, 30, 3, Lu, Tao* ..................................... 71

V. Joint Institute for Particle Nuclear Physics & Cosmology ........................................................................ 71 (189) On Dark Energy Models of Single Scalar Field, JOCAP, 2012, 04, Li, Mingzhe

* ................................... 71

(190) Search for Dark Matter Signals with Fermi-LAT Observation of Globular Clusters NGC 6388 and M15,

JOCAP, 2012, 04, Feng, Lei* .............................................................................................................................. 72

(191) Metric-Affine Formalism of Higher Derivative Scalar Fields in Cosmology, JOCAP, 2012, 07, Li,

Mingzhe* ............................................................................................................................................................. 72

VI. Other....................................................................................................................................................... 73 (192) A Study on the Celestial Phenomena and Chronology Recorded in the Ancient Text and the Modern Text

of the Bamboo Annals, AcASn, 53, 2, Zhang Jian* ............................................................................................ 73

(193) A Study on Marss Stay at Twenty-eight Lunar Mansions, Four-planet Conjunctions and Five-planet

Conjunctions during Past Dynasties of China, AcASn, 53, 4, Zhang Jian*........................................................ 73

紫台历年发表论文情况 .................................................................................................................................... 74

专著 .................................................................................................................................................................... 74

获奖 .................................................................................................................................................................... 74

专利 .................................................................................................................................................................... 75

紫台主要科研项目统计 .................................................................................................................................... 76

学术报告 ............................................................................................................................................................ 77

中国 2012 年度“十大天文科技进展” .............................................................................................................. 83


VIII

Annual Research Report’2012

1

2012 年度科研工作总结

一、科研工作总体情况

1. 概述

2012 年，紫台共有在研项目 240 项（包括新

增项目 109 项）。其中，主持国家重点基础研究发

展计划（973）项目 1 项和子项 3 项；主持（或承

担）中国高技术研究发展计划（863）项目 21 项（新

增 15 项）；主持（或承担）国家其他项目 21 项；

主持（或承担）国家自然科学基金项目 80 项（新

增 30 项），其中创新群体 1 项、重大项目 1 项（新

增 1 项）、重点项目 6 项（新增 1 项）、主任基金项

目 4 项、面上项目 28 项（新增 9 项）、杰出青年基

金 2 项，承担国家自然科学基金重大科研仪器设备

研制专项 1 项（新增 1 项）；承担中科院空间科学

战略先导科技专项 5 项（新增 2 项），主持（或承

担）中科院知识创新工程重要方向项目 5 项（新增

1 项），“百人计划”项目 6 项（新增 2 项），承担

重大国际合作项目 2 项（新增 1 项）；承担江苏省

自然科学基金 12 项（新增 5 项）；横向项目 13 项

（新增 8 项）。

2012 年，紫台共发表科技论文 193 篇，其中

国际合作论文 76 篇。SCI 论文 128 篇，影响因子

3.0 以上的 71 篇，被引用 95 篇次；申请专利 5 件，

其中发明专利 5 件，申请软件著作权 2 件；专利授

权数 8 件，其中发明专利 8 件，软件著作权登记 1

件。紫台完成的《“高能电子宇宙射线能谱超出”的

发现》项目获得国家自然科学奖二等奖，作为成员

单位参加的“嫦娥二号”工程项目荣获国家科技进

步特等奖，另获得省部级科技进步二等奖 3 项（其

中 1 项排名第一）、三等奖 1 项。

2. 重大进展

1）战略性先导科技专项 A 类“暗物质粒子探

测卫星”项目进展顺利。完成有效载荷关键技术攻

关和电性件研制等，并通过欧洲核子中心束流标定

实验，为工程转阶段打下了良好的基础。

2）国家重大科技基础设施“十二五”规划项

目——中国南极天文台项目预先研究项目基本完

成，进入立项建议书阶段。

3）主持申请的 973 项目“利用南极巡天望远

镜在超新星宇宙学及太阳系外行星方面的前沿研

究”成功立项。参与申请的先导科技专项 B 类“超

导电子器件应用基础研究”成功立项，紫台是其中

项目一“超导量子效应探索与电子器件研究”的共

同组长单位。主持的国家重大仪器设备研制专项“太

赫兹超导阵列成像系统”和国家自然科学基金重大

项目“极端台址环境下的天文望远镜关键技术方法

研究”启动实施；

4）空间目标与碎片观测系统建设取得重要阶

段性进展。完成具有自主创新概念的大型多目标观

测设备——二代光电阵的研制和全系统调试，进入

试运行阶段，各项指标达到预期，大幅度提高了全

网的探测能力。参加了“天宫一号/神舟九号”空间

碎片预警监测等多项国家任务，受到各方好评，为

中科院争得了荣誉。

5）紫台自主确定“战神”小行星轨道，圆满

完成“嫦娥二号”再拓展交会试验任务。嫦娥二号

卫星成功飞越 4179 小行星“战神”图塔蒂斯，并

获得高分辨光学图像。这是我国首次实现对小行星

的飞越探测，也是国际上首次实现对“战神”的千

米级近距离探测。紫台负责的小行星测定轨工作为

此次任务提供了保障，测定轨水平再次得到实战检

验，获得各方好评。

6）太赫兹量子级联激光器技术研究取得突破

进展。在国际上首次实现了基于频率与功率同时稳

定 QCL 激光器的太赫兹外差混频接收机。

3. 重大成果

1、作为成员单位参加的“嫦娥二号”工程荣

获国家科技进步特等奖，紫金山天文台负责研制了

其中载荷之一“伽马射线谱仪”，并在再拓展交会试

验任务中负责小行星“战神”图塔蒂斯的测定轨工

作。


2

2、以常进研究员为主要完成人的科研成果

《“高能电子宇宙射线能谱超出”的发现》荣获国家

自然科学奖二等奖；

3、季海生研究员牵头和美国科学家联合在国

际上首次发现加热日冕的超精细通道，研究成果在

美国 NASA 官网发布。

二、研究活动进展

I. 暗物质和空间天文研究部

宇宙学、暗物质及高能天体物理研究

主要在宇宙学相关的课题开展了研究工作，包

括微波背景辐射、超新星、伽玛暴、再电离、暗物

质和暗能量等。本年度发表论文 4 篇，其中第一完

成单位 2 篇。主编的“现代天体物理”一书已基本

完成，是《中外物理学精品书系》中的一本，将由

北京大学出版社出版。

伽玛暴由于它们具有很高的光度，我们能观测

到距离我们很远的样本，通过它们可以了解高红移

处宇宙演化的性质。但伽玛暴的标准烛光关系远没

有 Ia 型超新星好，目前已知的伽玛暴的光度关系都

有很大的弥散，这成为当前运用伽玛暴来研究宇宙

演化历史的瓶颈。我们用我们最新编纂的伽玛暴的

样本对文献中常用的伽玛暴的标准烛光关系进行了

一个系统的研究，搜索已知的关系中可能的隐藏变

量，从而探索降低标准烛光关系弥散的可能。通过

研究我们确认了一个弥散更小的光度关系，同时通

过对我们的结果的分析，我们指出了对该问题进一

步研究的可能的努力方向（ApJ）。参加了在瑞典斯

德哥尔摩举行的 The Thirteenth Marcel Grossmann

Meeting，并在分会上做了邀请报告。尝试性地探索

研究了一种直接测量宇宙膨胀速率的可能方法，最

后得出否定的结论。还调研学习 Fermi 卫星的数据

处理，为下一步的工作做准备。

与南京大学李明哲合作研究了微波背景辐射数

据对各向异性的 CPT 破坏的限制，此工作已完成，

正在整理。研究了本地的低密度区对超新星宇宙学

参数拟合的影响，此工作正投稿中。并正在尝试研

究快速产生宇宙再电离过程的红移场方法。

在宇宙学与高能天体物理的研究中基本建立了

相对论超流体在宇宙学与中子星中应用的理论框

架，在暗能量、中子星内部物理、耗散结构等方面

可望完成一批工作。

培养研究生：1）用宇宙结构增长的数据研究了

暗能量的性质，相应的工作已发表在 Phys. Lett. B

上；2）研究了宇宙早期产生的 ultracompact dark

matter minihalo 中的暗物质湮灭对微波、X-ray、

Gamma-ray 波段的光子背景的影响，相应工作正在

投稿中（见 arXiv:1206.3750）。

宇宙伽马暴、中子星及相关物理研究

主要进行高能爆发性天体的理论和观测研究和

X 射线双星的研究。

1）在伽玛射线暴方向上取得了重要的进展。与

美国宾夕法尼亚州立大学张彬彬合作，利用光球层

模型同时自洽地解释了伽玛暴观测得到的 4 个经验

关系，包括“瞬时辐射峰值频率——光度”关系、

“瞬时辐射峰值频率——外流体初始洛仑兹因子”

关系、“瞬时辐射光度——外流体初始洛仑兹因子”

关系以及“瞬时辐射峰值频率——伽玛暴辐射效

率”关系。文章发表在 ApJ Letter，当年就得到 10

次左右的引用。《中国科学报》在 A1 版以要闻的形

式对这一进展进行了报道，同时科学网也以新闻的

形式作了转载。此外，我们在伽玛暴的分类，伽玛

暴爆发的总能量和形成率的宇宙学演化等多个方面

都取得一定进展，有数篇文章发表在 ApJ，MNRAS

等杂志上。

2）在 X 射线双星方向我们继续分析我们所获

得的光学数据（分光和测光），结合公开的 X 射线

数据，多波段研究 X 射线双星中的各种现象。本年

度我们除了使用兴隆 2.16 米和 80cm 望远镜获得了

一定量的数据，还使用丽江 2.4 米望远镜对我们的

目标源进行了观测。目前我们已经成功申请到了

2013 年度 2.16m 望远镜的观测时间。在学术研究上

我们分析了三颗 Be/X 射线双星长期的光学测光和

分光数据，发现了光学变化和 X 射线辐射之间的关

系，这些研究成果一些已经发表在 2012 年度的 ApJ

中，还有一篇文章已经投到了 ApJ。此外我们还利

用 RXTE 的公开数据研究了黑洞 X 射线双星

H1743-322 的能谱和时变性质，这一研究结果已经

投到 MNRAS。我们还分析了一批 INTEGRAL 源的


3

REM 红外观测数据，并将 IGR J16318-4848 的研究

结果整理成文即将投稿。

太阳高能及相关物理过程研究

本年度本团组围绕太阳高能物理及相关问题开

展工作，包括：太阳 X 射线研究、伽玛射线研究、

多波段研究、极区喷流、日冕物质抛射研究、相关

理论方面的研究、以及涉及探测方面的空间项目预

先研究和地面大日冕仪项目推进，取得较好进展。

主持的 973 项目年内通过中期评估，年内团组新立

项 1 个基金重点项目、1 个基金面上项目、一个省

基金面上项目、1 个先导专项空间规划研究项目。

另外引进高端外国专家和外国专家特聘研究员 1

人。在高能天体物理研究方面参与 1 个超新星遗迹

研究的基金重点项目。10 月份成功举办了首届中德

太阳物理双边学术研讨会。

1) 太阳高能物理方面：a）耀斑能量频率分

布研究（ApJ）。利用 GOES 软 X-ray 数据及 RHESSI

X-ray 数据得到 GOES 耀斑的热等离子体的温度、

发射度、体积，得到耀斑峰值时刻的热等离子体热

能。在计入对可能的耀斑峰值前热能损失的修正后，

得到代表 GOES 耀斑的总能量。通过对这部分能量

的频数分布的研究，我们发现其频数分布负幂律指

数为 2.3。如果这个数值可以向下延伸到纳耀斑段，

就足以解释宁静太阳的日冕加热。b）研究了一类上

升相 GOES 光变行为表现为显著指数增长特征的简

单耀斑，建立了这类简单耀斑的样本，为详细研究

有关物理过程奠定基础（天文学报）。c）围绕耀斑

伽玛射线的理论计算和观测分析。具体内容包括实

现了基于 TALYS 程序所开展的太阳伽玛射线能谱

计算，新的核反应截面数据库使得伽玛射线能谱的

计算变的更加完整；此外，结合 GEANT4 蒙特卡洛

模拟和理论计算所得结果，应用到 RHESSI 卫星观

测数据分析，发现康普顿散射效应在太阳伽玛射线

能谱中有一定的作用，并从中提取出耀斑加速粒子

能谱、中子俘获线形成深度、以及它们的时间演化

特性等信息（RAA）。d）GLE69 和 GLE70 的最新

研究结果，提供了比以往更加信服的一系列证据，

指出其一为耀斑加速，另一为 CME 激波加速

（ApJ）。

2) 太阳多波段及 CME 研究方面：a）基于

喷流在白光波段的观测，研究了极区喷流中粒子的

受力状况，得到粒子的初始速度分布和源区总动能

等信息（A&A）。b）利用 SOHO/LASCO, STEREO

A/COR 和 STEREO B/COR 三个日冕仪不同视角对

CME 的白光观测，发展了一种新的方法，得到 CME

在三维空间的外体积。CME 的三维位置可用来预测

其传播方向和速度，可为空间天气预报提供重要信

息。该工作还跟踪了 CME 从太阳到金星的速度演

化等（ApJ）。c）把发展的新方法和已有方法进行

比较，发现该方法有其优越性。主要体现在新方法

利用三个不同视角的同时观测，因而可以更好的约

束 CME 三维形态；并且由于该方法无需假设 CME

的形状，因而适用范围更广（Solar Physics）。d）针

对爆发事件中的能量问题，研究了一个活动区中爆

发现象的各个能量分量，利用新的数据和方法，能

量估算更可靠（ApJ 已接收）。e）利用 SDO 上 HMI

和 AIA 的观测数据，研究光球磁流浮现区的性质以

及上层大气对光球磁流浮现的响应特征。分析发现

浮现的时间尺度可以从 1 小时到十多个小时，浮现

的面积、正负极性间的距离、磁流增长率以及平均

场强等参数与浮现的磁通量呈现出弱的正相关特

性，而正负极性间的分离速度则呈弱的负相关特性。

EUV 波段辐射的增强相对于磁流浮现有明显的延

迟（几十到几百秒钟），温度越高的谱线，延迟的时

间越长。同时，EUV 波段辐射的增强（日冕的加热

程度）与浮现的总磁通量正相关（RAA）。

3) 太阳空间和地面计划预先研究方面：开

展了天基莱曼阿尔法望远镜的前期研究和相关工

作，与长春光机所签订仪器设计合同，与长光所和

西光所一起开展关键技术攻关，完成深空太阳天文

台莱曼阿尔法成像仪建议书；开展了中国日冕磁学

望远镜（COMTEC）的先期工作，完成其科学需求

和科学目标文档，与美国高山天文台和南京天光所

合作，开展大口径日冕仪的光机设计。今年 5 月，

前往高山天文台参加首届日冕磁学会议；确定地基

法布里-珀罗光谱诊断日冕仪科学目标和参数需求，

与长春光机所签订设计合同，将在近期完成初步光

学设计；空间预研项目“先进天基太阳天文台预先

研究”进展顺利，年内完成了中期评估，针对相关

载荷进行了初步设计和协调，即将完成项目建议书；

年内还就深空太阳天文台上的高能粒子探测，邀请


4

德国同行前来合作探讨，寻求国际合作可能性。

4) 在高能天体物理研究方面：协助南京大

学陈阳教授获得“超新星遗迹及其激波过程的多波

段研究”重点基金项目的立项。该项目是建立在去

年指导陈阳老师的学生李辉完成的一个工作的基础

上，今年通过与高能物理研究所袁强博士合作，我

们发现由激波主导的超新星遗迹的伽玛射线辐射能

谱指数和其背景等离子体的密度有很好的相关性。

该模型假设激波中的粒子加速过程对背景介质的属

性不敏感，该模型对现有超新星遗迹伽玛射线能谱

的成功解释意味着有关的粒子加速过程应该有很好

的收敛性，从而为建立激波粒子加速的理论模型打

下坚实的观测基础。目前，我们正和云南天文台的

杨初愿博士，南京大学的研究生张潇和袁强博士一

起进一步发展这一模型。

太阳活动的多波段观测研究

我们将方向定位在多波段的“高分辨率观测”，

一方面在这个领域作出世界水平的研究工作，另一

方面为未来的大设备培育出科学目标。我们利用国

际最先进的观测设备尤其是大熊湖天文台的NST，

国际最大口径的太阳光学望远镜。尤其是，在利用

该望远镜时，我们选了一个从来没有在大口径望远

镜进行成像观测的波段：中性氦的10830Å谱线，我

们为NST贡献了国内生产的10830Å滤光器，以至我

们能够分享NST的观测成果。至于赣榆望远镜，口

径虽然不大，我们所定位的高时间分辨率成像观测

也是国际前沿的方向，这样的安排和运作使得我们

的目前和未来几年的工作都会处在世界前沿。同时，

几年下来的成果会一定让我们知道我们今后的设备

该做什么。

1）国际首次得到太阳在10830Å波段的高分辨

率成像图，并由此发现加热日冕的能量通道，为著

名太阳物理难题“日冕加热问题”的解决提供了全

新的思路。

2）继续利用RHESSI资料，仔细研究了2005年9

月13日的耀斑热和非热能量的过程。

3）发现了太阳活动区磁能双幂律谱的分布

（ApJ已接受），这是接下来几年工作的生长点。

暗物质与空间天文实验室

1) 暗物质粒子探测卫星研制进展：作为载

荷总体单位，携中科大、近代物理研究所、高能物

理研究所、空间中心等单位共同完成了一件产品的

研制，两次试验的验证，三大关键技术的攻关。一

件产品：载荷完成了 1/4 面积（探测器高度，即辐

射长度与鉴定件一致）样机，确定载荷各分系统之

间的电接口、软件接口。两次试验：载荷桌面联试

（南京，7 月-9 月），验证了软硬件接口，同时利用

宇宙线对整个探测器进行标定；载荷束流试验（欧

洲 CERN，9 月-10 月），利用高能电子和强子对探

测器进行试验，结果表明整个探测器方案设计合理，

能够满足物理目标。三大关键技术：“塑闪晶体温度

形变适应结构设计与实现”；“BGO 晶体大动态范围

信号读出”；“多路 Si-PIN 匹配 VA 芯片实现低噪声、

宽动态(能量/幅度)测量”。至 2012 年底，三大关键

技术均已攻关总结并通过专家评审。

通过两个月电性件联试，验证了载荷内部各单

机的电接口协议，表明目前的电接口能够满足探测

器要求。通过宇宙线测试，初步验证了探测器能够

正常工作，为束流试验奠定了基础。经过了桌面联

试验证，各参研单位于 9 月底赴欧洲核子中心

（CERN）进行束流试验。整个束流试验测试了探

测器的各项性能（电子能量线性、能量分辨、强子/

电子簇射区分等），数据初步处理结果表明探测器对

电子的能量线性、能量分辨等指标基本达到预期。

据悉，本次束流试验是中国人第一次将自己如此大

型仪器运送到 CERN 进行束流试验，研制人员的团

结协作使得试验的顺利进行也给国际同行留下了很

好的印象。2012 年 10 月 26 日，“暗物质粒子探测

卫星”(DAMPE)有效载荷束流试验初步处理结果在

中国科学技术大学顺利通过评审。

2）嫦娥二号卫星方面：“嫦娥二号”卫星在轨

运行正常，实验室承担研制的有效载荷伽玛射线谱

仪随嫦娥二号升空绕月进行观测。伽玛射线谱仪是

探月工程“嫦娥二号”卫星主要的有效载荷之一，

经过技术改进，它采用了新型的溴化镧(LaBr3)闪烁

探测器技术，其能量分辨率相比“嫦娥一号”普通

闪烁探测器提高了近 3 倍，在能量分辨率、探测灵

敏度等方面均有大幅提高。这也是国际上第一次采


5

用该类型探测器进行深空探测。截止 2012 年底，相

关数据处理表明：利用嫦娥二号伽玛谱仪对月球表

面大型撞击坑及其周围溅射物放射性元素含量的观

测，月球表面东海与危海盆地在其形成时，撞击深

度应该到达了下月壳，撞击事件可能把月球深层次

的物质挖掘了出来。该成果将发表于 4 月 8 日

Scientific Reports 期刊上。

恒星结构、演化与脉动研究

围绕日震学和星震学理论研究开展。开普勒卫

星升天之后，红巨星星震观测获得迅猛的发展，出

人意料地发现了红巨星的 g 模振荡。我们也紧随开

展了红巨星 g 模振荡的研究，取得了某些重要进展，

理论上证实红巨星存在脉动不稳定的 g 模，并预期

随红巨星光度增大，g 模的脉动振幅也增大。

参加了 SONG 项目组几乎所有的学术活动，承

担了邀请报告和研究生及项目组成员的培训工作。

为项目组开设了《恒星脉动理论》为期一周的专题

讲座。

指导博士生利用我们的非局部对流理论太阳对

流区模型，完成了太阳绝热声速反演。较之传统的

“标准太阳模型”，我们的结果有了本质上的改善，

大大减小了观测与理论的矛盾。证实了我们的理论

预言：在太阳对流区底部，日震反演显示的相对“标

准太阳模型”绝热声速的突然升高是由构成“标准

太阳模型”所采用的局部对流理论造成的。因此采

用我们的非局部对流太阳模型取代“标准太阳模型”

作为日震反演的参考模型时，观测与理论基础的矛

盾自然而然大大减小，甚至完全消失了。日震反演

的结果是对我们非局部对流理论的一个极有力的支

持。

恒星对流理论是至今尚未完全解决和存在争论

的科学问题。在恒星结构、演化和脉动理论计算中，

国际上广为采用（几乎是唯一一种）的是所谓的混

合长理论。混合长理论并不是一种遵循流体力学方

程的对流的动力学理论，而只是一种唯象理论。其

最大的优点是物理上的直观性和应用上的简单性，

其缺点也是明显的。为此我们发展了一种非局部和

非定常的恒星对流的统计理论。其优点是它是根据

流体动力学方程和湍流理论导出的，因而有较为坚

实的物理基础，能较为精确的描述湍动对流的动力

学过程。其缺点是不如混合长理论那样直观，应用

上也更为复杂。它还未能完全取代混合长理论用于

恒星演化的所有问题，还只是在一个比较小的范围

内采用。在 convective overshooting zone 结构和太

阳与恒星类太阳振荡激发机制二个重要理论问题

上，我们同当今国际主流观点完全不同。日震学绝

热声速反演结果对我们的 convective overshooting

zone 结构是个有力支持。我们的观点开始获得国际

上的认同。

南极天文中心

2012 年度在南极科考、仪器建设、科学研究、

等各个方面都取得了显著的工作成果。结合中国科

学院紫金山天文台“十二五”规划的内容，南极天

文中心正在向着有影响力的国际研究中心强力买

进，并在“两暗一黑三起源”重大科学问题的研究

中逐步确立我国的优势地位，同时为“十二五”国

家重大科技基础设施建设候选项目中国南极天文台

的立项和建设铺垫坚实的基础。

南极科考方面，2012 年度南极天文中心参加了

国家组织的两次南极内陆科学考察，2011 年 11 月 3

日正式开始至 2012 年 4 月 8 日结束的第 28 次中国

南极科学考察队，和 2012 年 11 月 5 日正式开始的

第 29 次中国南极科学考察队。在两次科学考察中，

南极天文都是其中一个非常重要的科考工作内容。

第 28 次科考队天文组成员成功维护了南极冰穹 A

地区的科学设备，并于 2012 年 1 月在冰穹 A 地区

顺利安装了首台南极巡天望远镜 AST3-1.第 29 次科

考队天文组成员已经到达南极冰穹 A 地区，正在准

备维护现在的仪器设备，取回 2012 年的天文观测数

据，并为明年将要安装的第二台南极巡天望远镜

AST3-2 准备场地。

同时，为了更好的参加中国南极科学考察，并

顺利完成其中的南极天文科考内容，南极天文中心

于 2012 年准备筹划了中心内部成员的体能、野外训

练内容，训练计划书已经完成，并准备实施。可以

在中心内部提前选拔合格的科考队员参加中国南极

科学考察队。

仪器建设方面，经过小口径中国之星小望远镜

阵 CSTAR 的平稳过渡，计划建造的 50cm 口径的南

极施密特望远镜阵（南极巡天望远镜 AST3）的首


6

台望远镜已经成功安装在南极冰穹 A 地区，并顺利

运行。第二台望远镜也已经建造完成，并将于 2013

年初进行测试和调控。为南极天文在宇宙大尺度结

构、超新星和伽马暴、系外行星、变星、星系和活

动星系核等研究领域提供了优于现阶段其他地面天

文观测设备的科学数据。同时，为南极冰穹 A 地区

的科学设备添加了新的能源系统 PLATO-A，为南

极巡天望远镜 AST3 提供足够的能源支持。并设计

了新的数据存储系统，可以便捷安全的储存海量的

AST3 天文观测数据。

初步确定了昆仑暗宇宙巡天望远镜 KDUST 的

设计参数。KDUST 光学的初步设计是加上改正透

镜的反射式系统，观测视场大约 1 个平方度，观测

的波长范围为 3000 埃到 3-5 微米，覆盖到近红外波

段，可以进行近红外波段的巡天观测。第一代仪器

设备可只包括光学，红外设备等技术及方案成熟后

可以作为后续设备。位于焦平面的光学 CCD 将使

用美国半导体技术有限责任公司（STA）制造的

10K×10K 成像器或类似设备拼接而成，图象质量

将达到 1 平方度视场中 0.25 角秒内为 80%。指向精

度约 2 角秒，跟踪精度约 0.2 角秒每 30 分钟，灵敏

度将达到一小时的观测时间内（S/N 大于 5）g 波段

的极限 AB 星等为 27 等，全视场灵敏度 FWHM 将

达到 0.3 角秒。

对中国之星小望远镜阵 CSTAR 的改造和性能

提升，完成了故障检测。并对目标跟踪系统、偏振

观测设计及工控机的升级完成了初步的规划。为最

大限度的在冰穹 A最佳观测环境下使用现有天文设

备对亮源的光变及偏振研究提供了极佳的科学机

会。

为了更好的规范南极天文设备的研制、运行、

管理以及南极科考的准备与管理、天文观测数据及

成果的管理等，南极天文中心成功的制定并向国家

提交了“极地天文观测指南”。

科学研究方面，伴随着首台南极巡天望远镜

AST3-1 的成功安装和顺利运行，使用 AST3 数据在

不同的科学领域进行深层次的科学研究，正在有条

不紊的进行，顺利通过了 973 项目“面向南极冰穹

A 中国南极天文台建设的天文观测关键技术和天体

物理重大问题”，确立了以宇宙大尺度结构、星系

和活动星系核、超新星与伽马暴、恒星、系外行星

为主的研究领域。

在宇宙大尺度机构的研究领域中，已经明确了

如下四个研究方向：基本宇宙学参数测量、暗物质

性质研究、星系形成的统计研究、暗能量的宇宙学

检验。并完善了相关的数据处理软件。结合国内在

数值模拟和理论模型上的研究优势，为探讨暗物质

和暗能量、第一代恒星和星系的形成、星系的形成

和演化的一系列关键科学问题提供保障

在星系和活动星系和的研究领域中，已经明确

了如下 5 个研究方向：星系与活动星系核的共同演

化、活动星系核光变与能源机制、黑洞潮汐撕碎恒

星事件、活动星系核的成团性分析、活动星系核核

区几何结构。基于南极冰穹 A 的极佳观测环境，以

及每年长达四个半月的极夜事件，AST3 的光变曲

线质量将远优于其他地面观测设备得到光变曲线。

基于 SDSS stripe82 数据，对光变曲线特征研究的各

种软件程序已经基本成熟，可以马上对 2013 年四月

份得到的 AST3 首批科学数据进行处理。

在超新星和伽马暴的研究领域中，已经明确了

如下 6 个研究方向：极早期超新星事件的探测、超

新星巡天和多波段测光、利用大样本数据寻找更均

匀的 Ia 超新星子类开展暗能量研究、宇宙高红移伽

马暴、伽马暴余辉、新类型红外暂现源。利用即将

交付使用的首批和后续的 AST3 高质量数据，将对

宇宙学的参数限定，超新星的前身星及物理机制，

伽马暴的物理起源和机制提供比较明确的答案。部

分对超新星和伽马暴的预研工作正在进行中，可以

使得后续的 AST3 观测能够更加及时准确的发现研

究超新星和伽马暴。

在恒星的研究领域中，已经明确了如下两个研

究方向：南极天区全赫罗图恒星的星震学研究、南

极天区疏散星团星震学研究。利用 AST3 的高质量

测光光变曲线，获得对恒星结构和演化规律的全面

了解和认识。现阶段的科学研究主要基于 CSTAR

的观测数据，现有的数据处理程序已经基本成熟。

在系外行星的研究领域中，已经明确了如下两

个研究方向：掩食法探测系外行星、微引力透镜法

探测系外行星。并通过对 CSTAR 光变数据的研究，

完成了通过测光光变寻找系外行星的软件设计。长


7

期持续的南极天文测光数据，获得大样本的系外行

星，我们将更加深刻地理解行星系统的起源和演化。

深度结合南极巡天望远镜的科学规划，南极天

文中心主要成员提交了参加中国科学院倡导的天文

先导 B 项目组的意向，加速中国南极天文事业的发

展，加深不同学科、不同院系之间的紧密合作。

国际合作方面，已成功的和澳大利亚建立了良

好的长期的合作关系。在中国科学院的关怀和帮助

下，相关的备忘录和协议已经签订，澳大利亚方面

的天文望远镜提供中国南极天文科学研究的后续和

辅助支持，包括光谱观测，光学外的其他波段观测

等。同时南极天文中心正在积极寻求和智利方的合

作，以期能使用现阶段国际上最先进的地面观测设

备。在正在筹建的中智天文中心的框架下，已经和

智利方达成了初步的意向

2012 年度，在首台南极巡天望远镜成功安装和

运行的良好氛围下，8 月在云南省丽江市成功召开

了国际会议“南极巡天望远镜国际合作会议”，为中

国南极天文，特别是南极巡天望远镜的科学规划和

目标，在国际合作方面提供了一个良好的平台，为

后续中国南极天文的国际合作展示了良好的前景。

星系宇宙学和暗能量研究

本年度主要科研工作分为以下 5 个方面：不同

宇宙学模型下的星系成团性；利用星系观测限制温

暗物质模型；卫星星系的恒星剥离过程； X-ray 星

系团和光学群的对应关系；宇宙速度场的分布；类

星体的形成机制

本年度主要成果是星系形成模型的理论研究。

我们发现目前的星系形成模型预言了太多的小质量

卫星星系，导致星系的亮点相关函数在小尺度太高。

无论是宇宙学参数从 WMAP1 年到 3 年的结果，都

预言了太多的卫星星系。

我们运行了几组温暗物质的数值模拟，发现可

以利用星系的恒星质量函数和 Tully-Fisher 关系来

限制温暗物质的质量。以前对温暗物质的质量限制

主要来源于小尺度的物理，我的研究表明也可以用

大尺度上星系的性质来限制暗物质质量（ApJ 已接

受）。

星系中的恒星形成研究

与美国加州理工学院的合作者吕南姚博士等合

作申请得到 Herschel SPIRE/FTS 的观测时间，对一

批有明显恒星形成的近邻到高红移星系，进行

HCN, CS, CO 等分子的多跃迁谱线观测；对近邻的

普通主并合星系对进行 Herschel 中远红外的成像观

测.通过 LVG 模型拟合得到星系致密气体的物理性

质，研究 CO SLED，电离气体的性质，结合 Spitzer、

Herschel 红外望远镜的档案数据得出星系中远红外

与致密分子气体发射强度的相关关系。

获得 IRAM30 米的观测时间，从已经得到的

Herschel 观测的 70 个亮红外星系中选择 18 个旋涡

-旋涡星系对用 CO 1-0 研究早期并合状态的恒星形

成效率，研究恒星形成率什么时候会加强。

开展中高红移宇宙中黑洞吸积活动研究工作。

通过“有偿使用国外望远镜项目”获得位于美国亚

利桑那州的 6.5 米 MMT 大型望远镜 3 天的观测时

间（PI：郑宪忠），对基于 WISE 巡天和 UKIDSS

近红外巡天数据选出的尘埃遮蔽星系核进行光谱观

测，证认红移和研究光谱特征。利用红波段通道光

谱仪（red spectroghrap）对受遮掩的快速黑洞增长

进行研究。

与法国国家科学研究中心 Alain Omont 合作启

动联合项目，利用高红移 Herschel 强透镜效应的

亚毫米星系中的毫米波分子谱线系统的检查与

AGN 的连接处的恒星形成。

1）利用 CO 和 13CO 和 1.3 毫米连续谱在百 pc

尺度的空间分辨率，给出了 3 个亮红外星系和一个

远红外类星体的 SMA 观测的初步结果。结果显示

这些星系的分子气体分布在转动盘上，速度梯度范

围是~30 到 120 km s-1 kpc-1。与档案数据 CO（3-2）

比较，CO（3-2）/（2-1）比率的空间分布随星系的

分布显示了明显的变化。发现 VV 114 重叠区域的

亮温度比 VV 114E 核区的亮温度低，说明了这个区

域膨胀部分的分子气体是亚热的。

2）用 IRAM30 米观测了 19 个红外超亮类星体

(IR QSO) 的宿主星系，给出了 17 个有 CO 数据的

观测结果。孕藏在这些天体中的冷分子气体的范围

是(0.2-2.1) × 1010 Msun (αCO = 0.8 Msun (K km s-1


8

pc2)-1). 发现了 IR QSOs 分子气体的性质，如分子

气体质量，恒星形成效率(L FIR/L'CO)，和 CO（1-0）

线宽，与在近邻的超亮红外星系（ULIRGs）中的是

差不多的。对低红移和高红移的 QSO 的 CO 比较揭

示了所有 QSO 中的 LFIR 和 L'CO(1-0)都有紧密的相

关性。这说明，与 ULIRGs 相似，所有 QSOs 的远

红外发射主要来自恒星形成加热的尘埃，而不是活

动星系核（AGN），确定了 Spitzer 观测中红外谱得

到的结果。AGN 活动相关的总光度和 CO 线光度之

间的相关关系说明了恒星形成和 AGN 活动来自于

同样的气体，以及 kpc 尺度的恒星形成和非常小尺

度内中心黑洞的积累过程之间的相关关系。

3）给出了质量支配的主并和率的宇宙演化从

z=1 以来的统计学研究。样本是根据质量从

COSMOS 场中选出的密近主并和星系对（CPAIR）。

比较 CPAIR 样本和一个近邻 H 波段选择的星系对

样本得到的不同红移处的成对率随恒星的质量没有

明显的不同。函数 f pair = 10-1.88(± 0.03)(1 + z)2.2(±0.2) 对

成对率（pair fraction）的最好的拟合适当的展示了

宇宙的强演化。并合率的拟合的最好的演化函数是

R mg (Gyr-1) = 0.053 × (Mstar/1010.7 Msun )0.3(1 + z)2.2/(1

+ z/8). 这个并合率指出，z=1 以来的质量 M star ~

1010-1011.5 M sun 的星系正在经历～0.5-1.5 的并合率。

结果显示，对于 z<=1 的质量 M star >= 1010.5 M sun 的

大质量星系，包括正在恒星形成星系的主并和能够

引起椭圆和红安静星系（RQGs）的形成。另一方

面，主并和并不能引起小质量 M star <~ 1010.3 M sun

的 RQGs 和椭圆星系的形成。进行的量化的估计显

示主并和对最大质量（M star >= 1011.3 M sun）星系

的恒星质量积累有很大的影响，但是小质量星系的

恒星质量积累是由恒星形成支配。与质量决定的

（超）亮红外星系出现率相比较，结果给出主并和

频率与（超）亮红外星系出现率相当或这更高。

4）研究了 34 个近邻的矮不规则星系的多波段

的亮度轮廓。这些波段包括银河系演化探测器

（ GALEX ）的 FUV/NUV, UBV, 和 H α 和

Spitzer3.6μm 图像。这些星系组成了 LITTLE

THINGS 巡天的主要部分。通过用一完备的恒星形

成历史库，借助方位角平均的能谱分布图模型，得

到了恒星质量表面密度分布和在三个不同时标，0.1

Gyr, 1Gyr 和一个哈勃时标，平均的恒星形成率。

并发现样本中，约 80%，短波长得到的径向轮廓，

相对于年轻星族，盘的标长比年老一些的星族的长

波示踪的盘的标长要短。这说明恒星形成盘正在收

缩。另外，piece-wise 指数轮廓能很好的描述恒星

质量表面密度的径向分布，约 80%的星系外面的盘

的质量轮廓比内部区域的更深。这个特性给出了对

恒星质量面密度轮廓向下弯曲的自然的解释。一般

情况下，样本星系的内部盘中最近的恒星形成率和

恒星质量的比随半径变化常数。然而，样本中有约

35%的星系盘展示了负的斜率，这与假定的亮旋涡

星系所谓的由内向外的盘的增长的假定相反。小质

量的矮不规则星系中内部盘中恒星形成中心聚集的

倾向被解释为环境通过恒星反馈对他们的影响和规

则的敏感度的结果。

5）首次测量了潮汐矮星系的产率并估计了它们

在所有矮星系中所占的比重。利用 hst／acs 的深场

goods gems 图像数据以及 combo 17 的测光红移数

据，对位于 chandra 南场的一个并合星系样本从它

们静止光学波段进行了形态学分析并证认了其中的

潮汐矮星系候选者。据此估计出在质量大于 3×108-9

Msun，红移处于 0.5< z<1.1 处的有较长幸存时标的

潮汐矮星系产率是每十亿年，每单位共动体积内约

有 1.4×10-5 个。另外考虑到其他文献中给出的星系

并合率以及潮汐矮星系幸存率，结论表明，近邻宇

宙中只有很小一部分（约 10％）的矮星系是潮汐起

源的。样本中的潮汐矮星系平均来说其光学颜色比

它的宿主星系更蓝。对两个潮汐矮星系从光学到近

红外能谱的星族分析支持了在新诞生的潮汐矮星系

中存在年轻的星族，它的年龄时 400／200 百万年，

恒星质量占据了星系总恒星质量的 40％／26％。这

些结论与在近邻潮汐矮星系中发现的不连贯的恒星

形成历史一致。

6）利用 Sloan 巡天的光谱数据和 STARLIGHT

代码，给出了 75 个孤立的旋涡星系 Sb-Sc 内 bulge

部分的恒星分布的综合分析。发现样本中伪 bulge

和典型的 bulge 中主要分布着老年的恒星，质量权

重的平均年龄大约 10 Gyr。然而一般情况下，伪

bulge 中的恒星比经典 bulge 中的恒星年轻，二者区

别并不明显，这说明至少在这些孤立的星系中，紧

紧依靠他们的恒星的分布很难区分伪 bulge 和

bulge。伪 bulge 的恒星形成活动时标比 bulge 中的


9

恒星形成活动要长，这说明实际的演化在这种环境

中更加重要。结果显示与 bulge 相比伪 bulge 有更低

的恒星速度弥散，这说明典型的 bulge 比伪 bulge

更加弥散。

分子云与恒星形成研究

2012 年度本团组在分子云性质、年轻星团、年

轻星吸积和外流活动、原行星盘结构和演化等研究

方向进行了研究。申请并获得国家基金委重点项目

“银河画卷计划—CO 分子巡天”；“银河画卷计

划”项目实施顺利；继续完善南极 Dome A THz 望

远镜关于分子云与恒星形成以及原行星盘和太阳系

天体的科学目标研究；参加国家基金委重大科研仪

器设备研制专项“太赫兹超导阵列成像系统”项目；

参加“中等口径大视场光学望远镜”项目的前期准

备。

一） “银河画卷计划”进展顺利：利用 13.7

米望远镜，得到了 Aquila Rift 区域超过 30 平方度

的优质数据。完成了 Aquila Rift、Rossete 等区域的

数据处理。于 8 月 20-31 日在北京召开的“第 28 届

国际天文学联合大会”上，展示了初步的研究成果，

相关论文正在撰写中。

二） M17 恒星形成区近红外偏振研究：对大

质量恒星形成区 M17 进行了大视场（~8'× 8'）近

红外 JHKs 成像偏振观测。点源的偏振角分布有 2

个峰值，分别在 170° 和 110°，表明 M17 中的磁场

结构是非均匀的。我们发现星团中的磁场方向为南

北向，而 HII 区中的磁场方向为 100°-140°，与银

盘基本垂直。这一形态表明在星团形成过程中，星

团中的磁场从原初方向发生了偏转。我们测量得到

该区域南部棒状结构的磁场强度为 ~ 230μ G，磁

场方向与天空平面的夹角为 40°。我们还发现 M17

恒星形成区中年轻星外流方向与磁场方向的相关性

很弱，这表明在 M17 中，磁场不是决定原恒星旋转

方向的主要因素（PASJ）。

三）原行星盘尘埃性质研究：为了研究原行

星盘中气体尘埃的分布和演化，针对类太阳恒星过

渡盘（盘中气体快速减少阶段的星周盘），通过国

际合作完善了原行星盘辐射转移 MC3D 模型，在此

基础上完成了 24 万个过渡盘年轻星的模型 SED 库

建造。应用这一模型 SED 库，对 69 个观测较为完

备的过渡盘年轻星的观测 SED 进行了拟合，得到了

这些过渡盘及其中心星的物理参量，例如盘的形态、

内外半径、盘的质量、尘埃大小等。由于原行星盘

辐射转移的数值模拟包含多个物理参量，难以建造

网格足够小的模型 SED 库。为了能够对观测 SED

在参量空间中进行充分的搜寻以寻找到最佳拟合，

我们将模拟退火（Simulated Annealing）方法应用于

年轻星过渡盘观测 SED 的拟合中。通过比较我们发

现模拟退火方法可以得到更好的结果。论文已经被

RAA 接受(Liu, Madlener, Wolf, Wang, 2013 in

press)。使用模拟退火方法对 DoAr 33 的观测 SED

进行了拟合，发现该过渡盘中存在尘埃向盘的中面

沉降的证据。该天体是使用 ALMA 等设备细致研究

行星形成初始过程的理想目标（A&A）。对近邻ε

Cha 星团，使用自己取得的 Spitzer/IRS 光谱资料和

VLT/VISIR 成像资料，结合文献资料，计算了星团

成员的年龄和质量。对两个极低质量恒星

USNO-B120144.7 和 2MASS J12005517，发现它

们的能谱分布总体偏低，盘中尘埃可能发生了沉降。

我们发现在ε Cha 这一稀疏星团中，原行星盘物质

耗散速度远低于密集星团。通过对 IRS 光谱 10 μm

特征的分析，发现所有星团成员的原行星盘都存在

尘埃增长和结晶化（A&A）。

四）小质量年轻星吸积活动的观测研究：利

用 Spitzer GLIMPSE 和 2MASS 对恒星形成区

NGC6357 所取得的公开红外测光数据，以及项目组

成员合作者所取得该恒星形成区中心区域 Spitzer

深度成像资料，并结合 X 射线波段资料，搜寻了该

恒星形成区的年轻星。使用 VLT /VIMOS 光学光谱

观测，获得了这些年轻星的光谱型，结合理论模型

得到了年轻星的质量和年龄。在 NGC6357 恒星形

成区我们新发现 2 个年轻星团。我们发现该区域最

大质量年轻星 Pis 24-1 是一个双星系统，其伴星是

该系统中主要 X 射线源。得到了该星团的初始质量

函数（IMF），发现该星团初始质量函数与猎户座

Trapezium 星团的初始质量函数很一致。使用 HST

档案资料，在 Pismis 24 星团中发现 5 个原行星盘

(proplyd)，其中 4 个为新发现。发现 Pismis 24 星团

的原行星盘总体出现频率约为 30%，比具有类似年


10

龄的星团的原行星盘总体出现频率低很多。对 19

个具有不同年龄和不同大质量星含量的星团，通过

对它们的原行星盘总体出现频率的分析，我们发现

在具有极大质量恒星的星团中，原行星盘物质被耗

散的速度是不具有极大质量恒星星团的两倍。在

Pismis 24 星团中我们还发现，在离 Pis 24-1 投影距

离小于 0.6 pc 范围内，原行星盘出现频率(19%)远低

于距离较远处的频率(37%)。据此我们提出，在

Pismis 24 星团中，邻近大质量恒星电离紫外光子照

射和光致蒸发的联合作用，引起了原行星盘磁−旋

转不稳定性的增强和吸积活动增强，从而使盘中物

质的耗散加快。这是关于大质量恒星强辐射场对邻

近原行星盘寿命影响的最具有系统性的研究

（A&A）

五）小质量年轻星质量外流活动的观测研

究：为了研究外流的运动学特征，对ρ Oph 恒星形

成区的核心区域进行了近红外深度成像，探测到 38

个近红外波段外流，其中 6 个是新发现。利用该区

域以往的成像资料，分析得出外流中 86 个氢分子近

红外发射特征的自行，自行速度范围为 8 －

140km/s，典型速度为 35 km/s。利用自行数据，可

靠地证认了外流的激发源，得出了外流的尺度、张

角以及外流速度随到驱动源的距离的变化，发现在

ρ Oph 区域原恒星驱动外流的比例与 T Tauri 恒星

驱动外流的比例接近，这表明在恒星形成的原恒星

和 T Tauri 这两个不同阶段，外流出现频率没有显

著变化。以往的观测结果是，原恒星阶段外流出现

频率高于 T Tauri 星阶段。我们分析认为这是由于

以往观测的灵敏度较低，导致强度较弱的 T Tauri

星外流未能完备地观测到。论文已投 A&A。根据审

稿人意见已经完成了修改。

六）系外行星大气研究：通过 TAP 项目在

2012 年 9 月获得了系外行星 HAT-P-1b 大气的透射

光谱；申请到 2013 年度 Hale P200/DBSP 望远镜对

系外行星 WASP-48b 的观测时间。

毫米波与亚毫米波技术实验室

主要包括：1）修购专项“太赫兹超导探测器研

制平台一期”建设与试验运行， 2）南极 Dome A 天

文选址用太赫兹傅立叶分光频谱仪运行与观测数据

处理，3）南极 5 米太赫兹望远镜关键技术预研究，

4）太赫兹频段超导非相干探测技术研究，5）太赫

兹高灵敏度超导探测器技术相关应用研究。

1）南极 Dome A 5 米太赫兹望远镜（DATE5）

关键技术预先研究取得实质进展。完成了南极

Dome A 5 米太赫兹望远镜（DATE5）天线的两项概

念设计；完成 1.4THz 波段超导 HEB 混频器单元原

理芯片的研制，性能处于国际前沿水平；完成 2GHz

带 FFTS 宽带高分辨率数字频谱仪的初步研制。另

外，初步完成南极 5 米太赫兹望远镜（DATE5）系

统和分系统的方案设计，开始太赫兹本振源和 4K

低温制冷等关键单元的初步试制。

2）“太赫兹超导探测器研制平台一期”建设成功

并开始试验运行。完成“太赫兹超导探测器研制平

台一期”的建设，于 2012 年 5 月 22 日通过中科院

计划财物局修购专项管理办公室组织的验收。该平

台包括三个系统：超导及金属薄膜磁控溅射系统、

绝缘层磁控溅射系统和掩膜对准光刻系统。运行迄

今，已经成功溅镀包括 Nb、Al、SiO2 在内的单层

或多层薄膜，重点制备的 Nb 膜溅射速率可以通过

改变直流电流或者射频功率进行良好控制，2 英寸

Nb 膜的厚度分布不均匀性约为 1.3%，石英基板上

溅镀的 Nb 膜也达到了接近 9.5K 的临界温度。

3）太赫兹量子级联激光器技术国际合作研究：

针对未来南极太赫兹计划及空间应用计划，与荷兰

SRON/TUDelft、美国 MIT 等研究组共同开展了太

赫兹量子级联激光器（QCL）技术的合作研究，中

方主要成员为任远（中欧联合培养博士生）和史生

才。利用更为先进的三阶分布反馈式量子级联激光

器和更具实用价值的闭环制冷器，基于太赫兹气体

吸收谱线成功实现了对太赫兹 QCL 激光器的频率

锁定和幅度稳定。研究成果发表于 Appl. Phys. Lett.

(98, 231109, 2011 & 101, 101111, 2012)，任远获得

2012 年度中科院院长特别奖。

4）太赫兹频段超导非相干探测技术研究：系统

研究了超导 HEB 微桥（类 TES）的直接检波性能，

以及两种平面天线直接检波频率响应的实测与模拟

仿真，成功制备分别基于 Ti 和 NbSi 薄膜的两种超

导 TES 探测器件。与荷兰 TUDelft 大学合作，完成

了集总参数结构和共面波导 meander 线结构两种基


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于 NbTiN 超导薄膜的动态电感探测器（MKIDs）的

设计和模拟仿真，Q 因子均高达 10k。利用高精度

EBPG 图形行程技术，成功制备两种基于 Si 基板的

MKIDs 器件。另外，完成了 0.3K 低温测试系统的

初步构建。

4）太赫兹高灵敏度超导探测器技术相关应用研

究：完成了 0.1-1.5THz 螺旋天线耦合 NbN 超导 HEB

混频器的设计仿真与器件制备，并完成了其噪声温

度特性与 FTS 特性的初步实验表征，显示了良好的

宽带性能。该项研究为宽频带太赫兹测量平台的研

制奠定重要基础；针对 NbN 超导 SIS 隧道结，开展

了详尽的直流与太赫兹探测特性研究，获得了不同

温度下的探测器特性。另外，初步研究了不同临界

温度超导 HEB 混频器噪声温度的温变特性，在 T/Tc

高达 0.8 时均显示良好噪声特性。该项研究为太赫

兹超导探测器在空间等极端环境的应用打下良好基

础；提出了基于单一超导 HEB 热电子混频器同时实

现太赫兹信号源锁相和太赫兹信号相干检测的系统

方案。针对一个 847.6 GHz 固态信号源开展了实验

演示，实现了该本振信号源的锁相，实测接收机噪

声温度变化仅由附加波束分离器引入。演示实验还

发现：由于采用了高灵敏度超导 HEB 热电子混频

器，在极低太赫兹参考信号源功率下，仍可实现良

好的锁相性能。该方法也适用于其他太赫兹信号源，

为后续开展太赫兹量子级联激光器的锁相打下基

础。

青海观测站

13.7 米望远镜全年开机运行 324 天，其中对外

开放课题观测 290 天。2012 年度新受理课题观测申

请 14 件，安排国内外申请的课题观测 17 件，完成

CO、HCO+、CH3OH 等几十条分子谱线的课题观

测。2012 年度望远镜平均每天扫描 1 平方度的天区。

2012 年度无论在设备运转、开放课题观测时间，还

是在设备稳定运行、数据产出量方面，继续保持历

史高位，数据质量则有更大提高。

更换了超导成像频谱仪系统的部分像元的

HEMT 放大器、 SIS 混频器重组，HBT 接头拧紧

补焊，减少干扰噪声，改善接收机的稳定性；更换

了大功率 UPS 不间断电源电池组，确保“银河画卷

计划”工作顺利进行。截止到今年年底，“银河画卷

计划”巡天工作已观测 1460 个巡天单元（每个单元

30′×30′），其中 2012 年度完成 1077 个巡天单元，

数据质量完全符合标准。

在国际重大天文研究计划贝塞尔 BeSSeL

Survey (Bar and Spiral Structure Legacy Survey)项目

中扮演重要角色。探索银河系棒和旋臂结构，即

BeSSeL 项目，已被美国国立射电天文台列为未来

10 年的重点项目，紫金山天文台是这个项目的主要

参与者之一，项目已经从 2010 年开始执行。在未来

5-7 年内，每年 VLBA 的 20%的观测时间将用于该

的项目，观测时间超过 5000 小时。2011 年，BeSSeL

项目第一轮观测已经结束，数据处理和分析已经完

成，正在整理成文，初步显示结果激动人心，经典

的银河系结构模型将被抛弃。徐烨在 IAU287 次天

体脉泽专门会议上被邀请作题为“甲醇脉泽和天体

测量”的特邀报告，标志着我国在这个领域已经达

到世界一流水平。另外，VLBA 的一个重大项目

BR129，研究成果以青海站科研人员作为 PI 发表，

其结果显示，大质量恒星形成区存在大的异常运动，

这对传统的密度波理论是一个重大挑战。

空间目标与碎片观测研究中心

2012 年度团组在科研、重大设备研制、完成国

家任务以及观测网的持续运行等各方面开展了大量

工作。

2012 年中心参加了多项国家任务，受到各方好

评。主要包括：①中俄火星探测器（萤火一号）陨

落期预报任务；②“天宫一号/神舟九号”空间碎片预

警监测任务；③863 中高轨监测任务；④俄罗斯微

风 M 火箭体爆炸碎片监测任务；⑤我国遥感卫星组

合舱监测任务；⑥我国长征四号乙火箭陨落期预报

任务；⑦国内火箭发射减缓技术评估。特别在中俄

火星探测器（2012 年 1 月）陨落期预报国际联测活

动中，根据 IADC 事后公布的结果报告，中心预报

精度在参加联测的 10 个组织中名列前茅，而且中心

预报结果及时上报国内有关部门，为国家和民众提

供了服务；在“天宫一号/神舟九号”空间碎片预警监

测任务中，中心全网观测设备采集的观测数据，占

整个观测数据的一半以上，其中大椭圆轨道空间碎

片的数据量占 80%以上，保障了“天宫一号/神舟九

号”的飞行安全，发挥了不可替代的重要作用，为我


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院争得了荣誉。

院配套基建项目顺利进行，已完成全部内容建

设，包括姚安、乌鲁木齐、洪河的观测楼等配套设

施。

30 厘米项目中，乌鲁木齐子阵已完成安装、调

试工作，全系统已进入试运行观测阶段。

2012 年 4 月、7 月，新一代空间碎片观测系统

的建设方案分别列入了国防科工局空间碎片专家组

的“十二五”空间碎片地基监测能力建设规划、中国

科学院空间碎片监测能力建设“十二五”规划方案

中，推动了新一代空间碎片观测系统的立项工作。

继续深入开展轨道长期演化规律、大气模型改

进、新目标关联、空间碎片搜索方法、天基探测与

识别方法研究、光度变化测量方法及其特性等方面

的研究工作。

建立了任意倾角小偏心率人造卫星的地球非球

形引力摄动的平运动轨道共振的统一理想模型。给

出了同步轨道带物体的扩展化理想共振模型，基于

该模型详细探讨了同步轨道空间碎片的二维相平面

结构及其稳定性，给出了二维相平面结构的主要特

征参数，理论上分析了常规面质比同步轨道物体的

轨道半长径和经度的稳定范围，并数值验证了相关

结果。探讨了不同倾角常规面质比近圆同步轨道物

体的相平面结构，并分析了相应相平面结构差异的

根源。同时，对半同步轨道的轨道共振问题、Molniya

和 Tundra 型轨道的双重轨道共振问题进行了理论

研究；对 Molniya 型轨道大面质比空间碎片的长期

动力学演化进行了数值模拟研究。

研究了高层大气模型的短期修正方法。现阶段，

在近地卫星轨道预报中，大气密度模型是一种重要

的误差来源。这一方面是由于高层大气的变化原本

就比较复杂，另一方面也与模型建模的固有缺陷有

关，是近地卫星预报中不可回避的难题。提出了利

用星载高精度大气实测资料对大气密度模型进行短

期近实时地修正，给出了四种合理的修正函数，应

用于一段较短时期的轨道预报。研究表明，方法能

较好地适用于中等和剧烈太阳辐射，以及磁暴的情

况，使得轨道预报精度提高 7%以上，个别案例中

能提高精度 30%以上。

卫星精密定轨及应用研究

CCD 相机研制实验室

完成了拼接 CCD 相机的初步性能测试。拼接

CCD 相机的成像靶面比较大（152mm×152mm）,

我台没有这么大的光学成像系统，于上海天文台联

系，使用佘山 1.56 米望远镜进行测试，测试结果表

明：拼接 CCD 相机在多口（20 个读出口）抗干扰、

长线传输（50 米千兆网）、读出噪声、暗流等方面

的性能指标都能达到预期的要求，为拼接 CCD 相

机实际使用打下了坚实的基础。

完成了大靶面高速读出 CCD 产品化生产的前

期准备，该大靶面高速 CCD 相机可用于替换国外

的 CCD 相机在大光电阵上的应用。实验室准备批

量生产该型号 CCD 相机以满足将来第二台光电阵

的需求；完成了小光电阵 CCD 相机（U6）的产品

化生产的准备，准备 2013 年批量生产，以取代洪河

小光电阵 CCD 相机的更新（该计划已申请到了修

购专项的支持）。

完成了 10G 光纤传输的 CCD 相机的设计，为

更高速的 CCD 相机研制奠定了基础。

积极参加小行星深空探测载荷方面的方案调研

和讨论；积极参加我台中等口径望远镜方案的调研

和讨论。

近地天体探测和太阳系天体研究

本年度团组主要开展了彗星观测和研究，并围

绕小行星深空探测开展了系列调研、研讨和相关研

究工作，参与编写《月球与深空探测》（小行星深空

探测手册），参与中科院行星科学实验室筹备和组建

工作。研究远距离彗星的活动性及其活动机制，分

析研究了 2011 年 4 月获取的 4 颗彗星的观测数据。

深入调研了特洛伊小行星的形成和演化的研究现

状，对其轨道演化及形成稳定区域的机制进行了初

步分析研究。主持和参加的国家自然科学基金项目

进展情况良好。团组 1 人次执行公派计划，赴美国

加州大学洛杉矶分校(UCLA)进行学术访问，2 人分

别参加了在北京召开的第 28 届 IAU 大会、在印度

召开的第 39 届 COSPAR 科学大会和美国天文学会

行星科学分会（DPS meeting）会议，提交会议报告

3 篇。接待了芬兰同行来台进行合作研究，在小行

星形状重建的分析方法合作研究方面取得了重要进


13

展。

研究远距离彗星的活动性及其活动机制，对

2011 年 4 月获取的 4 颗彗星的观测数据进行了处

理，发现彗星 29P/Schwassmann-Wachmann 和

C/2006 S3 位于较大的日心距（大于 3AU），仍有较

强的活动性，有明显的彗发；彗星 228P/2009 U2 的

活动性较小，具有恒星外观，而彗星 C/2009 K3 由

于亮度较弱，没能探测到。通过测光研究，获取了

彗星的表面亮度轮廓和表面亮度变化梯度；计算出

了彗核的半径上限；得出反映彗星活动性的参数

Afrho 值和质量生成率。

历算和天文参考系研究

在完成天文历书编算工作的同时，就航海导航

中历书天文学应用的电子化和标准化开展了广泛调

研工作，并在此基础上向海军有关部门提交了项目

建议书。在天体高精度运动理论及其相关领域开展

了多方面的研究工作，主要包括：国际上有关观测

资料的收集整理和归算验证工作、自主观测工作、

有关设备研制的调研工作；以建立完整的太阳系大

天体数值历表自主拟合软件系统为主要目标，开展

了适用拟合方法和可靠性检验方法的调研、实现和

在相对简单的双星和多星系统中的应用研究工作；

在相对论天体测量方面和历书天文学应用等方面完

成了若干研究工作。

完成了电子航海天文历的研制工作，并撰写了

详细的使用手册，在此基础上与海军出版社形成了

编制“航海天文历”编算标准的决定，同时与海军

航海保证部达成了航海天文导航软件系统研制的意

向，并提交了有关项目建议书。

开展了太阳系主要天体数值历表用观测资料的

收集整理和归算验证工作。主要进展包括：收集整

理了目前国际上各历表研制团队所采用的运动学观

测资料，数据总量近 60 万条，包括自上世纪初以来

有关外行星的方位资料，自上世纪 60 年代以来的内

行星和月球的测距资料，以及近几十年来航天器跟

踪测距和测速资料，此外还有把有关动力学参考架

连接到国际天球参考架所需的 VLBI 测角数据。对

上述方位测量数据编制了完整的归算软件，在利用

国际上现有历表验证有关数据的过程中，我们发现

部分数据存在明显的由观测资料预处理过程带来的

系统差，在如何合理地消除这种系统差方面开展了

一些初步研究工作。此外也开展了有关测距数据归

算模型建立方面的研究工作，尽管该工作有待进一

步完成，但已有初步结果发表。此外，开展了有关

自主观测资料获取方面的调研工作，并在此基础上

申请到了国家自然科学面上基金项目的支持，同时

参与了本台中等口径大视场望远镜科学目标工作

组，就历书天文和天文参考系的观测现状和需求开

展了调研工作并参与组织了有关咨询会议。

研究了太阳活动周期和行星运动周期之间的关

系，给出了两者之间存在多种周期对应关系的重要

结论,有关论文“Tang & Cheng Zhuo：The mid-term

and long-term solar quasi-periodic cycles and the

possible relationship with planetary motions.”已为杂

志 AP&SS 接受。

基于依巴谷中间天体测量资料，开展了单谱线

分光双星系统轨道拟合工作，首次得到或改进了 72

个系统的可靠光心轨道解，有关工作（Ren shulin, Fu

Yanning. Hipparcos Photocentric Orbits of 72

Single-lined Spectroscopic Binaries）已投 AJ，并已

提交了修改稿，审稿人对修改稿提出了两点简单的

修改意见，并同意在修改后予以发表。此外还开展

了分光双星视向速度观测研究工作，借助兴隆 2.16

米望远镜，对一些有兴趣的系统进行了光谱观测，

得到了多个双星的视向速度数据，后续研究正在开

展中。

围绕相对论参考系、相对论性引力理论以及高

精度历表研究，特别是相对论框架下行星际光传播

开展了多方面的研究工作，在标量张量理论框架下

建立了一种 2 阶后牛顿光传播模型。

利用我们建立的恒星经验质光关系，通过收集

可靠的恒星光度资料给出了子星为主序星的双星系

统的动力学视差和质量星表，拟给出一个计算动力

学视差相对简单有效的经验公式，相关结果正在分

析整理中。

此外，在天体力学基础理论和应用研究中本团

组研究生还分别开展了 1+n 体问题特解稳定性和嵌

埋星团质量分层方面的研究工作。


14

太阳和太阳系等离子体研究

2012 年度负责和参加承担的科研任务主要有：

（1）幂律谱电子回旋脉泽辐射机制的研究；（2）动

力学阿尔文波及其湍流的产生和激发机制的研究

（国家自然科学基金面上基金项目）；（3）太阳和太

阳系基本等离子体理论研究；（4）日地空间天气预

报的物理基础与模式研究。

主要在以下几个方面取得了一定进展：

1）太阳载流冕环中动力学阿尔文波的激发

和产生机制：我们近年来的系列研究工作显示动力

学阿尔文波在日冕加热问题中可能起重要作用，而

动力学阿尔文波在太阳磁等离子体大气环境中的激

发和产生机制一直是其中一个重要的关键问题。本

年度我们在这一关键问题的研究上取得了一些重要

进展，发现载流冕环中的场向电流能非常有效地驱

动动力学阿尔文波不稳定性并进而激发和产生动力

学阿尔文波。而这些动力学阿尔文波的波粒相互作

用能为载流冕环的加热提供有效的微观物理机制；

2）太阳磁等离子体大气中束流－回流系统

的动力学：高能带电粒子束流是天体爆发活动中最

普遍的观测现象之一，它们在磁等离子体环境中的

传播会引起一系列复杂的微观等离子体不稳定性过

程和动力学演化现象。本年度我们结合太阳硬 X 射

线耀斑的观测，深入分析了高能电子束流在太阳大

气中传播引起的束流－回流系统的动力学，发现在

一定条件下回流电流能有效地激发粒子声波并进而

导致束流电子能量的反常（非碰撞）损失。有关结

果能合理地解释太阳硬X 射线环顶源和足点源能谱

指数之差大于标准薄－厚靶模型观测预期的反常现

象；

3）太阳射电辐射机制的研究：射电辐射机

制是所有天体物理辐射机制中最复杂的一种，太阳

射电辐射无疑是人类能最清楚喜子地研究的宇宙射

电辐射现象。近年来，我们在电子回旋脉泽辐射的

微观物理机制的研究上驱动力一系列的重要进展，

特别是本年度我们的工作显示它们可能在太阳射电

辐射机制的问题中起重要的根本性作用，成为各类

太阳射电辐射现象共同的和根本的微观物理机制。

天体化学和行星科学实验室

主要开展了行星化学基础科学研究工作，参与

中科院“行星科学重点实验室”筹建工作，具体如

下：

1) 开展钙长辉长无球粒陨石的锆石定年工

作：对 Millbillillie, Camel Donga, NWA 6594 钙长辉

长无球粒陨石进行了矿物岩石学分析工作，找到了

数颗锆石矿物，利用北京地质所的 Cameca 1280 离

子探针，开展了 U-Pb 定年分析工作，获得了高精

度、高分辨率的年龄数据，三块陨石是目前太阳系

内最古老的玄武岩，与太阳系的年龄接近，形成于

太阳系的最初期。

2) 开展月海玄武岩的岩相成因研究：对

NWA 4734 玄武质月球陨石进行了矿物岩石学分

析，微量元素地球化学，和斜锆石 U-Pb 定年分析

工作，确定了岩相特征和成因机制，获得了高精度

的结晶年龄数据，发现了月壳岩浆演化过程中的混

染现象，为研究月球火山活动历史提供了重要证据。

3) 开展火星火山地质活动历史研究：对我

国在南极地区收集到的第二块火星陨石 GRV

020090 进行了矿物岩石学，微量元素地球化学，和

斜锆石 U-Pb 定年分析工作，发现 GRV 020090 是一

块富集型二辉橄榄岩质火星陨石，是全世界发现的

第二块这种类型的火星陨石。其中的斜锆石结晶年

龄为 2 亿年，说明火星在近期还存在岩浆活动的迹

象，否定了火星在 40 亿年前就停止了火山活动的论

点。

盱眙天文观测站

围绕中央级修缮购置项目“近地天体望远镜终

端升级改造”项目，主要进行了近地天体望远镜终

端升级为 10k*10kccd 系统，进行望远镜焦面装置更

新，以实现 4k 和 10kccd 相机的兼容，望远镜的光

学镀膜，圆顶大修等。另外近地天体望远镜运期间，

继续开展太阳系天体巡天观测研究，反银心方向多

色巡天观测研究，小行星光变曲线巡天，取得了良

好的效果。在此基础上拓展了更多的大视场巡天观

测计划，主要进行了反银心方向窄波段多色巡天观

测研究，低银纬区域宽带多色巡天和超新星巡天观

测研究的测试观测和巡天观测策略和数据处理方案


15

的讨论。本年度的设备升级为了配合小行星地面观

测研究和小行星深空探测的地基观测保障，升级后

可以更高效地进行太阳系天体的观测研究，从而促

进小行星探测项目的实施。

1) 完成了修缮购置项目“近地天体望远镜

终端升级改造”的大部分。基本完成了焦面设施的

升级，于 12 月 30 日进行测试观测；完成了滤光片

的定制；完成了近地天体望远镜数据库系统的建立

和发布（www.cneost.org）；10kccd 终端由于外商 STA

公司的原因预计延迟到 2013 年 1-2 月交付。

2) 继续开展小行星和近地天体搜索观测，

上报 MPC 共 2897 个太阳系小天体（包括小行星、

彗星和卫星）的数据共计 7 千余次，获得正式编号

小行星 85 个。

3) 开拓了小行星时序测光观测和研究，获

得了 106 个小行星的 255 条光变观测数据，得到了

一百多个小行星的光变周期。发展了一种快速椭球

反演算法，提出了一种新的计算小行星表面光度值

的积分方法，并通过应用 Lebedev 数值积分来快速

求解，进而利用 Levenberg-Marguartdt 算法来求解

非线性优化问题来寻求最优解。采集了小行星的多

次冲的光变曲线后，利用 Kaasalanen 等人发展的高

斯反演法和最优估计反演法建立了 4 个小行星的形

状模型。组织开展了盱眙、Kitt Peak 90cm 望远镜和

智利 60cm 望远镜对小行星 4179 的联合观测，取得

了支撑嫦娥二号再拓展任务的重要数据。

4) 完成了反银心方向巡天观测，完成了以

银河系反银心方向为中心、赤经 3 至 9 小时、赤纬

负 10 度至正 60 度约 5600 平方度的天区以及覆盖仙

女座大星云、三角座风车星云（除银河系外，构成

本星系群的另外两个主要漩涡星系）约 600 平方度

的扩展天区开展了 CCD 成像测光观测，以获取该

区域中天体的亮度和颜色，预期将产生包含约一亿

颗银河系恒星的星表，为后续的郭守敬望远镜光谱

巡天计划提供高精度的输入星表。成像观测使用了

斯隆巡天计划 g（绿）、r（橙）、i（红）三色滤光片。

初步数据分析表明，测光巡天定位精度达到 80 毫角

秒，测光精度达到 2%，与美国斯隆巡天相当。探

测极限星等约 19.3 等。

行星科学与深空探测实验室（筹）

参加了嫦娥二号卫星再拓展试验任务，对小行

星图塔蒂斯的测定轨精度进行了详细地分析、对飞

越时刻拍照策略及预期小行星成像效果进行模拟仿

真。我们还紧密配合卫星总体工作，对嫦娥二号卫

星在轨对月成像结果、卫星的惯性姿态和拍照策略

等进行多方面复核。为嫦娥二号近距离飞越小行星

提供了重要的科学依据和任务保障。

在小行星深空探测方面，不断深化小行星深空

探测任务科学目标和有效载荷论证工作，组织了有

机组分分析仪采样方案会议、有机组分分析仪器研

制研讨会等多次会议，积极推动了小行星深空探测

的进程。例如就我国首次小行星深空探测任务中关

键载荷之一“有机组分分析仪”的工程技术指标和探

测性能指标进行了反复深化论证，已于 2012 年 12

月正式启动了有机组分分析仪的原理样机研制工

作，预计 2013 年年底将能完成整机的研制和相关论

证试验。围绕小行星深空探测主题，积极展开各项

调研和研究工作，主要包括：小行星形状建模和表

面温度建模、小行星引力场模型、小行星空间环境

研究、小行星雷达探测、近红外波段小行星成分探

测、小行星表壤研制、深空探测自主导航研究任务、

小行星形成与演化等，不断深化《小行星深空探测

科学手册》的内容。

继续开展行星科学基础研究工作，系统地研究

了在一些行星系统中的类地行星动力学演化和形成

机制、内部结构等。共完成了 13 篇研究论文。

1）系外行星动力学方面: 利用数值模拟方法

对 Vega 系统的碎片盘和可能存在的行星进行了模

拟。模拟中的碎片盘位于 80~120 AU，盘中尘埃尺

寸从 10 µm-100 µm，轨道偏心率与倾角都很小。通

过多组计算结果发现，如果 Vega 系统中不存在行

星，那么碎片盘演化结果与最新的观测结果吻合得

较好；如果存在行星，且行星偏心率较大（比如

e=0.6）时，行星的轨道半长轴不能大于 60 AU，否

则碎片盘会在行星的影响下产生明显的聚集现象，

行星与碎片盘的 2:1 平运动共振是导致碎片盘产生

结构的主要原因。

2）行星形成方面:（1）研究了 KOI 152 系统

1:2:4 共振构型。数值模拟得出了该系统形成过程中


16

可能经历的几个阶段：首先在距离目前位置较远的

系统外部区域成长为目前质量大小的行星胚胎；然

后在气体盘未消散前经过轨道迁移过程到达目前的

观测位置，在此过程中三颗行星胚胎相继进入 1:2:4

共振构型；最后通过与中心天体的潮汐作用将行星

胚胎的轨道圆化，从而形成具有较小偏心率并且脱

离轨道共振的三颗行星。讨论了形成这种构型系统

满足几个条件：系统中三颗行星均未经历过第二类

轨道迁移；行星的质量上限分别为 16.14、27.37 和

38.86 个地球质量；系统中恒星具有低吸积率或磁场

较强的特点等；行星胚胎的第一类轨道迁移速度应

低于线性理论估计值的十分之一等。经历过上述三

个阶段且满足相关条件后系统将形成与目前观测到

的 KOI152 系统相似的构型。（2）对热木星系统

WASP-50，热超级地球系统 GJ 1214 和类地双行星

系统 CoRoT-7 的潮汐演化过程进行了深入研究。研

究结果表明，恒星对行星的潮汐效应使行星的轨道

衰减和圆化，使行星演化至当前的轨道。由于潮汐

演化的最终轨道与系统的初始轨道有关，根据 GJ

1214b 目前的偏心率上限值(0.27)，模拟结果给出了

它在采用的模型中最大的初始偏心率值(0.4)。对

GJ1214 系统，还研究了选取不同潮汐耗散因子 Q’

时的演化过程，结果表明 GJ 1214b 的实际 Q’可能

远大于典型的类地行星的取值，合理地解释了 GJ

1214b 目前还存在着较大的偏心率，而且正处于缓

慢的圆化过程中。对于双行星系统的 CoRoT-7，潮

汐效应使两颗行星的轨道都经历了衰减和圆化，在

轨道演化过程中，潮汐效应与伴星的引力摄动效应

相互耦合，共同影响着两颗行星最终的轨道。（3）

研究了 Kepler-10 系统的潮汐演化过程。在动力学

模型中主要考虑了中心恒星作用到内行星上的潮汐

效应和相对论效应，以及两颗行星之间的引力摄动。

结果发现，Kepler-10b 由于非常靠近中心恒星，潮

汐衰减和圆化现象极为明显，潮汐效应对内行星轨

道演化的最后构型起非常重要的塑造作用。根据该

系统潮汐演化过程的研究结果，我们还推测了该系

统在潮汐演化以前的可能图像：内行星可能经历了

行星与行星之间的散射过程，从而获得了显著的偏

心率值；而外行星可能是从原行星盘中迁移到目前

的位置附近，由于气体对偏心率的抑制作用，它维

持了接近于零值的偏心率。

3）行星内部结构方面:研究了木卫二的内部结

构。对木卫二的内部进行了建模计算，考虑到木卫

二的质量较小，除了 Fe 和 FeS 内核外，还建立了

以推测的火星内核成分 Fe-FeS 混合物为内核的模

型。三个模型均分为核、幔和液态水三层，它们之

间的区别在于组成内核物质成份。模型一的内核由

Fe 构成，计算得到的总半径 1562 km, 其中内核半

径 431 km，硅酸盐幔 999 km，液态水层 132 km。

模型二的内核由 FeS 构成，总半径 1563 km, 其中

内核半径 777 km，硅酸盐幔 619 km，液态水层

167km。模型三的内核由 Fe-FeS 混合物构成，总半

径 1569 km, 其中内核半径 571 km，硅酸盐幔 832

km，液态水层 166km。上述模型的主要差别在于内

核的比例。具有最大内核的是模型二，其内核约占

半径的一半；具有最小内核的是模型一，其内核不

到半径的 30%。

4）系外行星观测方面:利用盱眙观测站 1 m 巡

天望远镜，对 HAT-P-12 b，TrES-3 b，WASP-3 b，

WASP-12 b，WASP-43 b，XO-1 b、TrES-3 等多个

系外行星目标作多次掩星观测并获得数据，已处理

了 TrES-3 b 及 WASP-43 b 的数据并获得光变曲线,

关于 TrES-3 的结果已发表在 AJ 上。

5）太阳系小天体研究方面:研究了 Damocloids

族群的动力学演化过程。从统计结果上得到

Damocloids 的两个可能起源：位于 Kuiper 带之外的

散射盘及位于 2000-20000 AU 之间的 Oort 云。来

自散射盘的 Damocloids 主要是通过与太阳系内大

行星的相互作用而被散射到接近地球的位置。存在

三个原因可能导致 Oort 云中的天体成为

Damocloids：与经过太阳系的恒星的作用；银盘的

潮汐作用；可能存在的太阳伴星的影响。首次提指

出来自 Oort 云的 Damocloids 有一个共同的特点：

即在演化过程中将经过位于 700-1000 AU 的过渡

盘。在研究的 Damocloids 成员中 37%的可能来自散

射盘，而 63%倾向于来自 Oort 云。

三）学术交流与合作

1. 国际合作与交流概况


17

2012 年度紫金山天文台全年实际出访人员为

159 人次（会议、项目合作研究、考察、观测、博

士生学习等），其中一年以上 4 人次，3 个月以上

2 人次，涉及美国、英国、法国、德国、俄罗斯、

西班牙、芬兰、意大利、日本、韩国、澳门及香港

等 17 个国家和地区。全年来访 152 人次，分别来

自美国、英国、法国、德国、俄罗斯、芬兰、荷兰、

日本、丹麦及台湾等 10 个国家及地区。引进“青

年千人计划”1 人，获批中科院“外国专家特聘研

究员”2 人、“外籍青年科学家” 2 人、高端外国

专家 1 人。与美国、德国、法国、荷兰等国科研院

所联合培养博士生 23 人。截止 2012 年 12 月 5 日，

与国际合作同行联合发表论文约 73 篇，2012 年度

用于国际合作与交流的经费约为 270 万元。主办国

际会议 4 个，参会国外学者近 60 人次。

2. 国际合作项目进展

1）恒星形成研究、太赫兹技术以及南极天文

方面

与德国马普天文研究所、马普射电天文研究所、

基尔大学、波鸿大学、美国 CfA、日本名古屋大学

等就银河系分子云巡天、恒星形成的最新成果开展

了广泛合作研究。多渠道争取国际先进观测设备的

使用时间，取得了高质量的观测资料。通过国际合

作，得到 Herschel SPIRE/FTS 和 IRAM30 米及位

于美国亚利桑那州的 6.5 米 MMT 大型望远镜的观

测时间，促成星系中的恒星形成研究取得更多的新

进展。继续开展国际大型计划 Bessel 合作研究。

与荷兰代尔夫特理工大学（TU Delft）签署了

科学与技术合作谅解备忘录，双方继续在超导 KID

探测器的研制方面开展合作，并希望能共同推动建

立中荷太赫兹天文与技术合作研究中心。与荷兰空

间技术研究所、巴黎天文台及莫斯科师范大学合作

研究了 1.4THz 频段的 NbN 超导热电子混频器，

取得 800K 的接收机噪声温度。与法国空间与天体

物理研究所合作，进行超导TES 探测器的合作研究。

举办了太赫兹超导探测技术研讨会。

中国南极天文研究发展迅速，已得到国际社会

的广泛关注。2012 年 8 月中国科学院与澳大利亚

天文联合组织在北京签署了关于南极天文合作的谅

解备忘录。主办“2012 南极巡天望远镜国际合作

会议”，有自中国、美国、澳大利亚、日本等国家近

100 位专家和学者参加，就南极科学考察情况，南

极巡天望远镜研制、运行与控制，科考数据处理与

分析，南极天文前沿科学研究，2012-2013 年度南

极天文科考工作，第 2、3 台南极巡天望远镜设计

建造、科学研究以及合作协调等多个课题展开了广

泛的交流与深入的讨论。。分别与德国 MT

Mechatronics公司和美国Simpson Gumpertz &

Herger 公司合作完成南极 5 米太赫兹天线的概念

设计。

“星系形成与宇宙大尺度结构”中德马普伙伴

小组正式启动，在马普伙伴小组的框架下，扩大双

方的合作，重点开展银河系形成研究和大尺度结构

的数值模拟研究。举办了“星系形成与宇宙大尺度

结构”中德双边会议。

2）暗物质与空间天文探测技术、太阳物理研

究以及宇宙伽玛暴研究方面

2012 年中日宇宙线科学观测合作取得很大进

展。日本 CALET 探测器研制进展顺利，目前已完

成多项试验。中方对其提供的模拟分析也在试验中

得到验证。利用欧洲核子中心（CERN）的高能质

子/电子束对暗物质粒子探测器进行标定，测试暗物

质粒子探测器的性能（能量分辨，粒子种类区分本

领等），取得了预期效果。日内瓦大学具有的较为成

熟的技术，满足了我们探测卫星对硅探测器的需求。

2013 年将继续与瑞士方面合作，对硅阵列探测器

的联合研制进行细化讨论。

继续执行中科院国际合作项目“莱曼 α 轨道望

远镜（LYOT）样机关键技术合作研究”，探讨空间

日冕仪科学、技术方案及在仪器研制中可能的合作。

开展与美国高山天文台合作，进行地基大口径日冕

仪的设计工作，并准备初步设计评估材料。

国际知名的高能天体物理专家 Melia 教授作为

我台特聘研究员，协助完成了中国科学院空间科学

战略性先导科技专项“暗物质粒子探测卫星”的前

期科学准备工作。与俄罗斯空间研究所签署了

2013-2014 中俄太阳物理合作研究计划，继续开展

太阳高能物理中俄合作项目。

与俄罗斯普科瓦天文台签署了交流合作协议，

在太阳活动的射电理论方面开展合作，2012 年聘

请了 Melnikov 教授为特聘研究员，在耀斑的射电

辐射机制方面进行指导，合作发表论文。与美国大


18

熊湖天文台已经保持了十多年的合作，主要瞄准了

该台当时正在建设的国际最大的光学望远镜 NST，

NST 于 2009 年出光。通过国际合作首次获得

10830Å 高分辨率成像观测，发现了加热日冕的超

精细通道，这一发现有望解决“日冕加热”问题。

研究成果入选国家基金委今年的亮点工作。

主办首届中德太阳物理双边学术研讨会，约 70

余位代表参加了会议。

3）空间目标与碎片观测研究方面

2012 年组团参加第 63 届国际宇航大会，介

绍用图像重叠技术探测大椭圆轨道空间碎片以及光

学空间碎片观测中形态数学应用方面的最新研究成

果。利用会议的各个场合，与欧空局、美国宇航局

的各位同行沟通了空间碎片碰撞预警，空间态势感

知，动目标识别等方面的最新进展。

4）行星科学方面和深空探测方面

开展彗星测光观测和研究工作，并利用位于夏

威夷的红外望远镜学习和实践红外观测方法；通过

国际合作在小行星形状重建的分析方法合作研究方

面取得了重要进展。利用近地天体望远镜，参加了

小行星和彗星的国际联测，磋商了将来参加 Gaia

太阳系天体后随观测网。计划与台湾鹿林天文台光

学观测设备的联合，进行彗星测光观测，并开展相

关研究。

继续开展碳质球粒陨石中富铝球粒和难熔包体

的矿物岩石学和氧同位素地球化学工作，利用美国

加州理工学院的离子探针仪，测试这些物体中的氧

同位素组成，探讨太阳系早期所发生的重要天文事

件。

Annual Report’2012–Abstract List of Publications in 2012

19

ABSTRACT LIST OF PUBLICATIONS IN 2012


20

I. Dark Matter & Space Astronomy

Record 1 of 193

Scientific Achievements of Prof. Chien Shiung Wu

Lu, Tan

Asia Pac. Phys. Newslett

卷: 1; 期: 2; 页: 52

Five years ago, we wrote two papers in memory of Prof. Chien Shiung Wu [1-2]. And now in memory of her 100th birthday, I am very happy to write this paper again. Indeed, she is a world top-class female experimental nuclear physicist. She is also known as the Chinese Madame Curie. As is well known, Madame (Marie) Curie was the first in discovering the radioactive substances, while C. S. Wu was the first in thoroughly studying β-decay, the most mysterious one among radioactivities. C. S. Wu did various experiments in proving the Fermi's theory of β-decay carefully and precisely, and even also improving it precisely and perfectly, and leading to the correct V-A form of the β-interaction and even leading to the electro-weak unification finally. Indeed, C. S. Wu known as Chinese Madame Curie is reasonable and admirable. As compared with Madame Curie, E. Segrè (1980) even said that C. S. Wu is more worldly, elegant, and witty [3].

Record 2 of 193

Constraining Dark Energy Using Observational Growth Rate Data

Shi, K.; Huang, Y. F.; Lu, T.

PHYSICS LETTERS B

卷: 717; 页: 299-306

Observational growth rate data had been derived from observations of redshift distortions in galaxy redshift surveys. Here we use the growth rate data to place constraints on the dark energy model parameters. By performing a joint analysis with the Type la supernova, baryon acoustic oscillation and cosmic microwave background data, it is found that the growth rate data are useful for improving the constraints. The joint constraints show that the ACDM model is still in good agreement with current observations, although a time-variant dark energy still cannot be ruled out. It is argued that the growth rate data are helpful for

understanding the dark energy. With more accurate data available in the future, we will have a powerful tool for constraining the cosmological and dark energy parameters.

Record 3 of 193

A Comprehensive Comparison of Cosmological Models from the Latest Observational Data

Shi, K.; Huang, Y. F.; Lu, T.

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY

卷: 426; 期: 3; 页: 2452-2462

We carry out a detailed investigation of some popular cosmological models in light of the latest observational data, including the Union2.1 supernovae compilation, the baryon acoustic oscillation measurements from the WiggleZ Dark Energy Survey and the cosmic microwave background information from the Wilkinson Microwave Anisotropy Probe seven-year observations, along with the observational Hubble parameter data. Based on the selection statistics of the models, such as the Akaike and the Bayesian information criteria, we compare different models to assess their worth. We do not assume a flat universe in the fitting. Our results show that the concordance Λ cold dark matter (CDM) model remains the best model to explain the data, while the Dvali–Gabadadze–Porrati model is clearly not favoured by the data. Among these models, the models whose parameters can reduce themselves to the ΛCDM model provide good fits to the data. These results indicate that for the current data, there is no obvious evidence to support the use of any more complex models over the simplest ΛCDM model.

Record 4 of 193

Toward Tight Gamma-Ray Burst Luminosity Relations

Qi, Shi; Lu, Tan

ASTROPHYSICAL JOURNAL

卷: 749; 期: 2; 页: 99-104

The large scatters of luminosity relations of gamma-ray bursts (GRBs) have been one of the most important reasons preventing the extensive application of GRBs in cosmology. Many efforts have been made to seek tight luminosity relations. With the latest sample of 116 GRBs with measured redshift and spectral parameters, we investigate 6 two-dimensional (2D) correlations and 14 derived three-dimensional (3D) correlations of GRBs to explore the possibility of decreasing the intrinsic scatters of the luminosity relations of GRBs. We find the

Cosmology, Dark Matter and High-Energy

Astrophysics


21

3D correlation of E-peak-tau(RT)-L to be evidently tighter (at the 2 sigma confidence level) than its corresponding 2D correlations, i.e., the E-peak-L and tau(RT)-L correlations. In addition, the coefficients before the logarithms of E-peak and tau(RT) in the Epeak-tRT-L correlation are almost exact opposites of each other. Inputting this situation as a prior reduces the relation to L alpha (E'(peak)/tau'(RT))(0.842 + 0.064), where E'(peak) and tau'(RT) denote the peak energy and minimum rise time in the GRB rest frame. We discuss how our findings can be interpreted / understood in the framework of the definition of the luminosity (energy released in units of time). Our argument about the connection between the luminosity relations of GRBs and the definition of the luminosity provides a clear direction for exploring tighter luminosity relations of GRBs in the future.

Record 5 of 193

Discrete Mass Ejections from the Be/X-Ray Binary A0535+26/HD 245770

Yan, Jingzhi; Li, Hui; Liu, Qingzhong


卷: 744; 期: 1; 页: 37-42

We present long-term optical spectroscopic observations on the Be/X-ray binary A0535+26 from 1992 to 2010. Combined with the public V-band photometric data, we find that each giant X-ray outburst occurred in a fading phase of the optical brightness. The anti-correlation between the optical brightness and the H alpha intensity during our 2009 observations indicates a mass ejection event had taken place before the 2009 giant X-ray outburst, which might cause the formation of a low-density region in the inner part of the disk. The similar anti-correlation observed around 1996 September indicates the occurrence of the mass ejection, which might trigger the subsequent disk loss event in A0535+26.

Record 6 of 193

Revisiting the Long/Soft-Short/Hard Classification of Gamma-Ray Bursts In the Fermi Era

Zhang, Fu-Wen; Shao, Lang; Yan, Jing-Zhi; Wei, Da-Ming


卷: 750; 期: 2; 页: 88-98

We perform a statistical analysis of the temporal and spectral properties of the latest Fermi gamma-ray bursts (GRBs) to revisit the classification of GRBs. We find that the bimodalities of duration and the energy ratio (E-peak/Fluence) and the anti-correlation between

spectral hardness (hardness ratio (HR), peak energy, and spectral index) and duration (T-90) support the long/soft-short/hard classification scheme for Fermi GRBs. The HR-T-90 anti-correlation strongly depends on the spectral shape of GRBs and energy bands, and the bursts with the curved spectra in the typical BATSE energy bands show a tighter anti-correlation than those with the power-law spectra in the typical BAT energy bands. This might explain why the HR-T-90 correlation is not evident for those GRB samples detected by instruments like Swift with a narrower/softer energy bandpass. We also analyze the intrinsic energy correlation for the GRBs with measured redshifts and well-defined peak energies. The current sample suggests E-p,E-rest = 2455x(E-iso/10(52))(0.59) for short GRBs, significantly different from that for long GRBs. However, both the long and short GRBs comply with the same E-p,(rest)-L-iso correlation.

Record 7 of 193

Gamma-Ray Bursts: The Isotropic-Equivalent-Energy Function and the Cosmic Formation Rate

Wu, Shi-Wei; Xu, Dong; Zhang, Fu-Wen; Wei, Da-Ming


卷: 423; 期: 3; 页: 2627-2632

Gamma-ray bursts (GRBs) are brief but intense emissions of soft gamma-rays, mostly lasting from a few to a few thousand seconds. For these types of high-energy transients, the isotropic-equivalent-energy (Eiso) function may be more scientifically meaningful than the GRB isotropic-equivalent-luminosity (Liso) function, as the traditional luminosity function refers to steady emission much longer than a few thousand seconds. In this work we construct, for the first time, the isotropic-equivalent-energy function for a sample of 95 bursts with measured redshifts (z), and find an excess of high-z GRBs. Assuming that the excess is caused by a GRB luminosity function evolution in a power-law form, we find a cosmic evolution of, which is comparable to that between Liso and z, namely (both 1s). The evolution-removed isotropic-equivalent-energy function can be reasonably fitted by a broken power law, in which the dim and bright segments are and, respectively (1s). The cosmic GRB formation rate increases quickly in the region of , remains approximately constant for , and finally decreases with a power index of -3.80 +/- 2.16 for z?4, in good agreement with the cosmic star formation rate observed to date.

Record 8 of 193

Multi-Wavelength Study Of the Be/X-Ray Binary MXB 0656-072

Yan, Jingzhi; Heras, Juan Antonio Zurita; Chaty, Sylvain; Li, Hui; Liu, Qingzhong


Gamma-Ray Burst, Neutron Star and

relevant physics


22

卷: 753; 期: 1; 页: 73-83

We present and analyze the optical photometric and spectroscopic data of the Be/X-ray binary MXB 0656-072 from 2006 to 2009. A 101.2 day orbital period is found, for the first time, from the present public X-ray data (Swift/BAT and RXTE/ASM). The anti-correlation between the Ha emission and the UBV brightness of MXB 0656-072 during our 2007 observations indicates that a mass ejection event took place in the system. After the mass ejection, a low-density region might develop around the Oe star. With the outward motion of the circumstellar disk, the outer part of the disk interacted with the neutron star around its periastron passage and a series of X-ray outbursts were triggered between MJD 54350 and MJD 54850. The Proportional Counter Array-HEXTE spectra during the 2007-2008 X-ray outbursts could be well fitted by a cutoff power law with low-energy absorption, together with an iron line around 6.4 keV, and a broad cyclotron resonance feature around 30 keV. The same variability of the soft and hard X-ray colors in 2.3-21 keV indicated that there were no overall changes in the spectral shape during the X-ray outbursts, which might only be connected with the changes of the mass accretion rate onto the neutron star.

Record 9 of 193

X-Ray and Optical Observations of A 0535+26

Camero-Arranz, A.; Finger, M. H.; Wilson-Hodge, C. A.; Jenke, P.; Steele, I.; Coe, M. J.; Gutierrez-Soto, J.; Kretschmar, P.; Caballero, I.; Yan, J.; Rodriguez, J.; Suso, J.; Case, G.; Cherry, M. L.; Guiriec, S.; McBride, V. A.


卷: 754; 期: 1; 页: 20

We present recent contemporaneous X-ray and optical observations of the Be/X-ray binary system A 0535+26 with the Fermi/Gamma-ray Burst Monitor (GBM) and several ground-based observatories. These new observations are put into the context of the rich historical data (since similar to 1978) and discussed in terms of the neutron-star-Be-disk interaction. The Be circumstellar disk was exceptionally large just before the 2009 December giant outburst, which may explain the origin of the unusual recent X-ray activity of this source. We found a peculiar evolution of the pulse profile during this giant outburst, with the two main components evolving in opposite ways with energy. A hard 30-70 mHz X-ray quasi-periodic oscillation was detected with GBM during this 2009 December giant outburst. It becomes stronger with increasing energy and disappears at energies below 25 keV. In the long term a strong optical/X-ray correlation was found for this system, however in the medium term the H alpha equivalent width and the V-band brightness showed an anti-correlation after similar to 2002 August. Each giant X-ray outburst occurred during a decline phase of the optical brightness, while the H alpha showed a strong emission. In late 2010 and before the 2011 February

outburst, rapid V/R variations are observed in the strength of the two peaks of the H alpha line. These had a period of similar to 25 days and we suggest the presence of a global one-armed oscillation to explain this scenario. A general pattern might be inferred, where the disk becomes weaker and shows V/R variability beginning similar to 6 months following a giant outburst.

Record 10 of 193

Gamma-Ray Bursts and Other Observations: Constraints on Cosmographic Parameters and Dark Energy Models

Liu, Jian-wei; Fa-yin Wang

Chinese Astronomy and Astrophysics

卷: 36; 期: 2; 页: 155-168

We use the newly released Union2 SNe Ia dataset to constrain cosmographic parameters, namely the deceleration, jerk and snap parameters (q0, j0 and s0), then calibrate the five luminosity relations of Gamma-ray Bursts (GRBs) at redshift z ≤ 1.4. Assuming that the GRB luminosity relations do not evolve with the redshift, we obtain the distance moduli of 66 high-redshift GRBs. At last, we combine the observational datasets including the observations of the Cosmic Microwave Background (CMB), Baryon Acoustic Oscillation (BAO) and the 116 GRBs with known redshifts to constrain some widely-discussed dark energy models. We find that the ΛCDM model is the best according to the Bayesian Information Criterion (BIC), and the JBP model is the best according to the Akaike Information Criterion (AIC).

Record 11 of 193

Analytical Afterglow Light Curves of Gamma-ray Bursts: the Case of a Flat Electron Spectrum

Wang, Y.; Fan, Y. Z.; Wei, D. M.; Covino, S.


卷: 36; 期: 2; 页: 148-154

In the standard afterglow model, the swept electrons

have a single power-law energy distribution dn/dγe ∝

γ−p e (p ∼ 2.3), owing to the first order Fermi acceleration process. However, in some events people find a lot of evidence for a flat electron spectrum (i.e., p < 2). In this work, the analytical afterglow light curves in the case of a flat electron energy distribution are presented respectively for a single power-law spectrum and a broken power-law spectrum, then the results are applied to the specific burst GRB 060908. Besides, we have also speculated a possible solution of the so-called low energy spectrum crisis of Gamma-ray Bursts.

Record 12 of 193

Early Afterglow Emission as a Probe of the Density Profile of the Medium Surrounding Gamma-Ray Bursts

Jin, Z. P.; Xu, D.; Covino, S.; D'Avanzo, P.; Antonelli, L. A.;


23

Wei, D. M.

Memorie della Societa Astronomica Italiana Supplement

卷: 21; 页: 194-197

The gamma-ray bursts (GRBs) with durations longer than 2 seconds, namely long gamma-ray bursts, are believed to have a massive star progenitor and should be born in the free stellar wind medium holding up to a radius > 1017cm. We propose to constrain the density profile of the medium with the early afterglow data and find out that for the interstellar medium (ISM) an early rapid increase of the afterglow flux is possible while in the free wind medium there is no such a signature. For GRB 060418 and GRB 060607A we show that the data is well consistent with the ISM model and the number density is low. While for GRB 081109A, the X-ray and optical data are consistent with the forward shock emission of an ultra-relativistic ejecta expanding into a wind bubble, in which the free wind terminates at a radius ˜ 4.5×1017cm, beyond which the medium is ISM-like. The implication of these results has been discussed.

Record 13 of 193

On the Frequency Distributions of Solar Soft X-ray Flares

Gan, W. Q.; Li, Y. P.; Feng, L.

EAS Publications Series

卷: 55; 页: 239-243

By giving three different definitions of peak flux(original peak flux, corrected peak flux, and scaled peak flux), we analyze the frequency distributions of 14057 flares recorded by GOES from 2000 to 2005. We find a significant result that the frequency distribution of the scaled peak flux for all the sample flares can be approximated by a perfect power-law function with an index of 2.18, without any usually deviating from the power-law at the lower fluxes.

Record 14 of 193

China’s Space Astronomy and Solar Physics in 2011-2012

ZHANG, Shuangnan; YAN, Yihua; GAN, Weiqun

Chinese Journal of Space Science

卷: 32; 期: 5; 页: 605-613

In the first part of this paper, we describe briefly the mid and long-term plan of Chinese space astronomy, its preliminary study program, the current status of satellite missions undertaken, and the current status of astronomy experiments in China’s manned space flight program. In the second part, the recent research

progress made in the fields of solar physics is summarized briefly, including solar vector magnetic field, solar flares, CME and filaments, solar radio and nonthermal processes, EUV waves, MHD waves and coronal waves, solar model and helioseismology, solar wind and behavior of solar cycle.

Record 15 of 193

The Calculation of Solar Gamma-Rays by TALYS

Chen, Wei; Gan, wei-qun


卷: 36; 期: 1; 页: 49-62

Solar gamma-ray lines, produced from nuclear reactions of accelerated particles interacting with the solar atmospheric medium, are the most direct diagnosis for the acceleration and transportation of energetic electrons and ions in solar flares. Much information about composition, spectrum, and angular distribution of the accelerated ions, as well as the elemental abundances of the ambient solar atmosphere can be derived from solar gamma-ray line spectra. A new gamma-ray calculation program has been developed by using an efficient nuclear code − TALYS. The theory of gamma-ray production in solar flares is treated in detail. The characteristics of gamma-ray spectrum are also presented.

Record 16 of 193

Ground-Based giant solar Telescope of China

Liu, zhong; Deng, yuanyong; Ji, haisheng; Li, Hui

Scientia Sinica Physica, Mechanica & Astronomica

卷: 42; 期: 12; 页: 1282-1291

Ground-based giant facilities with capabilities of both visible and infrared observations has played essential role in solar observation, to meet the requirement of the present-day solar physics and Space weather research. It significantly throws light on our understanding of the Earth-Sun relation and predicting its effects on the terrestrial environment. We firstly review the present status of the existing ground-based solar telescopes over the world and programs of new generation telescopes in USA and European countries. This paper aims to overview the project of next generation ground-based solar telescope of China, including its scientific goal, key techniques, experiments, site-survey and the current situation.

Record 17 of 193

Commission 12: Solar Radiation and Structure

Alexander Kosovichev; Gianna Cauzzi; Valentin Martinez Pillet; Martin Asplund; Axel Brandenburg; Dean-Yi Chou; Jorgen Christensen-Dalsgaard; Weiqun Gan; Vladimir D. Kuznetsov; Marta G. Rovira; Nataliya Shchukina; P. Venkatakrishnan


卷: 7; 期: T28A; 页: 81-94

High-Energy Solar Astrophysics


24

Commission 12 of the International Astronomical Union encompasses investigations of the internal structure and dynamics of the Sun, mostly accessible through the techniques of local and global helioseismology, the quiet solar atmosphere, solar radiation and its variability, and the nature of relatively stable magnetic structures like sunspots, faculae and the magnetic network. The Commission sees participation of over 350 scientists worldwide.

Record 18 of 193

An Observational Study on Coronal Hard X-ray Sources in Flares

Bai, Wei-dong; Li, You-ping; Gan, Wei-qun


卷: 36; 期: 3; 页: 246-260

Observational studies on solar flares with footpoints partially occulted by the solar limb provide an important method for diagnostics of coronal hard X-ray emissions. The statistics of hard X-ray sources in 71 such flares observed by RHESSI (Reuven Ramaty High-Energy Solar Spectroscopic Imager) show that the two kinds of hard X-ray sources proposed in previous studies (i.e., the sources with respectively a smaller and larger spatial separations between the thermal and non-thermal sources of coronal hard X-ray emissions) have no evident difference in the aspects of their photon spectra, images, light curves, GOES durations, etc. The area of the radiation region, the flare's total thermal energy and GOES duration are well correlated with the distance of separation. These results support some unified models of solar flares proposed in recent years, and indicate that the Masuda flare is only a kind of special event, which does not possess the general features of coronal hard X-ray emissions.

Record 19 of 193

An Attempt at a Unified Model for the Gamma-Ray Emission of Supernova Remnants

Yuan, Qiang; Liu, Siming; Bi, Xiaojun

The Astrophysical Journal

卷: 761; 期: 2; 页: 133-139

Shocks of supernova remnants (SNRs) are important (and perhaps the dominant) agents for the production of the Galactic cosmic rays. Recent γ-ray observations of several SNRs have made this case more compelling. However, these broadband high-energy measurements also reveal a variety of spectral shapes demanding more comprehensive modeling of emissions from SNRs. According to the locally observed fluxes of cosmic-ray protons and electrons, the electron-to-proton number ratio is known to be about 1%. Assuming such a ratio is universal for all SNRs and identical spectral shape for all kinds of accelerated particles, we propose a unified model that ascribes the distinct γ-ray spectra of different SNRs to variations of the medium density and the spectral difference between cosmic-ray electrons

and protons observed from Earth to transport effects. For low-density environments, the γ-ray emission is inverse-Compton dominated. For high-density environments like systems of high-energy particles interacting with molecular clouds, the γ-ray emission is π0-decay dominated. The model predicts a hadronic origin of γ-ray emission from very old remnants interacting mostly with molecular clouds and a leptonic origin for intermediate-age remnants whose shocks propagate in a low-density environment created by their progenitors via, e.g., strong stellar winds. These results can be regarded as evidence in support of the SNR origin of Galactic cosmic rays.

Record 20 of 193

Solar Flares with an Exponential Growth of the Emission Measure in the Impulsive Phase Derived from X-ray Observations

HAN, Fei-ran; LIU, Si-ming

Acta Astronomica Sinica

卷: 53; 期: 6; 页: 482-499

The light curves of solar flares in the impulsive phase are complex in general, which is expected given the complexities of the flare environment in the magnetic field dominant corona. With the GOES (Geostationary Operational Environment Satellite) observations, we however find that there are a subset of flares, whose impulsive phases are dominated by a period of exponential growth of the emission measure. The flares occurring from January 1999 to December 2002 are analyzed, and the results from the obervations made with both GOES 8 and 10 satellites are compared to estimate the instrumental uncertainties. The frequency distribution of the mean temperature during this exponential growth phase has a normal distribution. Most flares within the 1σ range of this temperature distribution belong to the GOES class B or C with the frequency distribution of the peak flux of the GOES low-energy channel following a log-normal distribution. The frequency distribution of the growth rate, and the duration of the exponential growth phase also follow a log-normal distribution with the duration covering a range from half a minute to about half an hour. As expected, the growth time is correlated with the decay time of the soft X-ray flux. We also find that the growth rate of the emission measure is strongly anti-correlated with the duration of the exponential growth phase, and the mean temperature increases slightly with the increase of the growth rate. The implications of these results on the study of energy release in solar flares are discussed at the end.

Record 21 of 193

Statistical Study of Emerging Flux Regions and the Response of the Upper Atmosphere

Zhao, Jie; Hui Li

Research in Astronomy and Astrophysics


25

卷: 12; 期: 12; 页: 1681-1692

We statistically study the properties of emerging flux regions (EFRs) and response of the upper solar atmosphere to the flux emergence using data from the Helioseismic and Magnetic Imager and the Atmospheric Imaging Assembly onboard the Solar Dynamics Observatory. Parameters including total emerged flux, flux growth rate, maximum area, duration of the emergence and separation speed of the opposite polarities are adopted to delineate the properties of EFRs. The response of the upper atmosphere is addressed by the response of the atmosphere at different wavelengths (and thus at different temperatures). According to our results, the total emerged fluxes are in the range of (0.44−11.2)×1019 Mx while the maximum area ranges from 17 to 182 arcsec2. The durations of the emergence are between 1 and 12 h, which are positively correlated to both the total emerged flux and the maximum area. The maximum distances between the opposite polarities are 7–25 arcsec and are also positively correlated to the duration. The separation speeds are from 0.05 to 1.08 km s−1, negatively correlated to the duration. The derived flux growth rates are (0.1−1.3)×1019 Mx h−1, which are positively correlated to the total emerging flux. The upper atmosphere first responds to the flux emergence in the 1600Å chromospheric line, and then tens to hundreds of seconds later, in coronal lines, such as the 171Å (T = 105.8 K) and 211Å (T = 106.3 K) lines almost simultaneously, suggesting the successive heating of the atmosphere from the chromosphere to the corona.

Record 22 of 193

The Past and Future of Space Solar Observations

GAN, WeiQun; HUANG, Yu; YAN, YiHua


卷: 42; 期: 12; 页: 1274-1281

After a brief review on the history of the international space solar observations, together with analyzing the current status in China, we elaborate in particular the recent strategic studies on Chinese space solar observations. Some candidates of the future missions are described, such as Deep-Space Solar Observatory (DSO), Advanced Space Solar Observatory (ASO-S), Solar Radio Array of Lower Frequency (SRALF), Stereoscopic Polarization Imager for Explosive Sun (SPIES), Super High Angular Resolution Principle for coded-mask X-ray imaging (SHARP-X), and High-sensitivity Observations of Solar High-Energy Radiation (HOSHER).

Record 23 of 193

The effect of Compton scattering on gamma-ray spectra of the 2005 January 20 flare

Chen, Wei; Gan, Wei-Qun

RESEARCH IN ASTRONOMY AND ASTROPHYSICS

卷: 12; 期: 10; 页: 1439-1459

Gamma-ray spectroscopy provides a wealth of

information about accelerated particles in solar flares, as well as the ambient medium with which these energetic particles interact. The neutron capture line (2.223 MeV), the strongest in the solar gamma-ray spectrum, forms in the deep atmosphere. The energy of these photons can be reduced via Compton scattering. With the fully relativistic GEANT4 toolkit, we have carried out Monte Carlo simulations of the transport of a neutron capture line in solar flares, and applied them to the flare that occurred on 2005 January 20 (X7.1/2B), one of the most powerful gamma-ray flares observed by RHESSI during the 23rd solar cycle. By comparing the fitting results of different models with and without Compton scattering of the neutron capture line, we find that when including the Compton scattering for the neutron capture line, the observed gamma-ray spectrum can be reproduced by a population of accelerated particles with a very hard spectrum (s <= 2.3). The Compton effect of a 2.223 MeV line on the spectra is therefore proven to be significant, which influences the time evolution of the neutron capture line flux as well. The study also suggests that the mean vertical depth for neutron capture in hydrogen for this event is about 8 g cm(-2).

Record 24 of 193

An Interpretation of the Possible Mechanisms of Two Ground-Level Enhancement Events

Firoz, Kazi A.; Gan, W. Q.; Moon, Y. -J.; Li, C.


卷: 758; 期: 2; 页: 119-131

We have carried out this work to clarify the possible mechanisms of two important high-energy particle events (GLE69 2005 January 20, 06: 46 UT and GLE70 2006 December 13, 02: 45 UT). For this purpose, the cosmic-ray intensities registered by neutron monitors at several sites have been analyzed and studied with concurrent solar flares of different energy bands. To determine whether the ground-level enhancement (GLE) might be caused by the energy released from a solar flare or a CME-driven shock, we identify the particle injection time in terms of the lowest value of the spectral indices deduced from proton fluxes. If the GLE is caused by the energy released from particle acceleration in a solar flare, the intensive phase of the flare representing extreme emission should lie within the injection time. While fulfilling this criterion, it is further necessary to understand the possible relativistic energy computed in terms of the possible travel time deduced by employing the observational time lag between the GLE and the concurrent solar flare. Accordingly, we have found that GLE69 is procured with sufficient possible relativistic energy (similar to 1.619 GeV) by the energy released from particle accelerations in the intensive phases of a solar flare components that have been corroborated by the injection time. The intensive phases of the flare components have also been justified with the prominent phases of a solar radio type III burst. For event GLE70, the particle


26

injection time lies within the CME-driven shock justified by a solar radio type II burst which seems to be capable of procuring sufficient possible relativistic energies (similar to 1.231 to similar to 2.017 GeV). It is also noted that any fractional amount of energy (similar to 0.226 to similar to 0.694 GeV) from preceding flare components might be considered as a contribution to the shock acceleration process. Thus, GLE70 is presumably caused by the sum of the energy released mostly from a CME-driven shock and partially from preceding flare components.

Record 25 of 193

Improvements to the X-ray Bremsstrahlung Thick-target Model and Their Applications to Solar Flare Observations

Su, Yang


卷: 53; 期: 2; 页: 181-182

In this dissertation, we focus on the improvements to the nonuniform ionization thick-target models and their applications to solar flare X-ray observations in deriving the non-thermal electron distribution, ionization distribution, and density distribution in flares.

Record 26 of 193

Particle kinetic analysis of a polar jet from SECCHI COR data

Feng, L.; Inhester, B.; de Patoul, J.; Wiegelmann, T.; Gan, W. Q.

ASTRONOMY & ASTROPHYSICS

卷: 538; 页: A34

Aims: We analyze coronagraph observations of a polar jet observed by the Sun Earth Connection Coronal and Heliospheric Investigation (SECCHI) instrument suite onboard the Solar TErrestrial RElations Observatory (STEREO) spacecraft. Methods: In our analysis we compare the brightness distribution of the jet in white-light coronagraph images with a dedicated kinetic particle model. We obtain a consistent estimate of the time that the jet was launched from the solar surface and an approximate initial velocity distribution in the jet source. The method also allows us to check the consistency of the kinetic model. In this first application, we consider only gravity as the dominant force on the jet particles along the magnetic field. Results: We find that the kinetic model explains the observed brightness evolution well. The derived initiation time is consistent with the jet observations by the EUVI telescope at various wavelengths. The initial particle velocity distribution is fitted by Maxwellian distributions and we find deviations of the high-energy tail from the Maxwellian distributions. We estimated the jet's total electron content to have a mass between 3.2 x 10(14) and 1.8 x 10(15) g. Mapping the integrated particle number along the jet trajectory to its source region and assuming a typical source region size, we obtain an

initial electron density between 8 x 10(9) and 5 x 10(10) cm(-3) that is characteristic for the lower corona or the upper chromosphere. The total kinetic energy of all particles in the jet source region amounts from 2.1 x 10(28) to 2.4 x 10(29) erg.

Record 27 of 193

Evolution of Hard X-Ray Sources and Ultraviolet Solar Flare Ribbons for a Confined Eruption of a Magnetic Flux Rope

Guo, Y.; Ding, M. D.; Schmieder, B.; Demoulin, P.; Li, H.


卷: 746; 期: 1; 页: 17-27

We study the magnetic field structures of hard X-ray (HXR) sources and flare ribbons of the M1.1 flare in active region NOAA 10767 on 2005 May 27. We have found in a nonlinear force-free field extrapolation over the same polarity inversion line, a small pre-eruptive magnetic flux rope located next to sheared magnetic arcades. RHESSI and the Transition Region and Coronal Explorer (TRACE) observed this confined flare in the X-ray bands and ultraviolet (UV) 1600 angstrom bands, respectively. In this event magnetic reconnection occurred at several locations. It first started at the location of the pre-eruptive flux rope. Then, the observations indicate that magnetic reconnection occurred between the pre-eruptive magnetic flux rope and the sheared magnetic arcades more than 10 minutes before the flare peak. This implies the formation of the larger flux rope, as observed with TRACE. Next, HXR sources appeared at the footpoints of this larger flux rope at the peak of the flare. The associated high-energy particles may have been accelerated below the flux rope in or around a reconnection region. Still, the close spatial association between the HXR sources and the flux rope footpoints favors an acceleration within the flux rope. Finally, a topological analysis of a large solar region, including active regions NOAA 10766 and 10767, shows the existence of large-scale Quasi-Separatrix Layers (QSLs) before the eruption of the flux rope. No enhanced emission was found at these QSLs during the flare, but the UV flare ribbons stopped at the border of the closest large-scale QSL.

Record 28 of 193

Statistical Analyses on Thermal Aspects of Solar Flares

Li, Y. P.; Gan, W. Q.; Feng, L.


卷: 747; 期: 2; 页: 133-140

The frequency distribution of flare energies provides a crucial diagnostic to calculate the overall energy residing in flares and to estimate the role of flares in coronal heating. It often takes a power law as its functional form. We have analyzed various variables, including the thermal energies E-th of 1843 flares at their peak time. They were recorded by both Geostationary Operational


27

Environmental Satellites and Reuven Ramaty High-Energy Solar Spectroscopic Imager during the time period from 2002 to 2009 and are classified as flares greater than C 1.0. The relationship between different flare parameters is investigated. It is found that fitting the frequency distribution of E-th to a power law results in an index of -2.38. We also investigate the corrected thermal energy E-c_th, which represents the flare total thermal energy including the energy loss in the rising phase. Its corresponding power-law slope is -2.35. Compilation of the frequency distributions of the thermal energies from nanoflares, microflares, and flares in the present work and from other authors shows that power-law indices below -2.0 have covered the range from 10(24) to 10(32) erg. Whether this frequency distribution can provide sufficient energy to coronal heatings in active regions and the quiet Sun is discussed.

Record 29 of 193

Morphological Evolution of a Three-Dimensional Coronal Mass Ejection Cloud Reconstructed From Three Viewpoints

Feng, L.; Inhester, B.; Wei, Y.; Gan, W. Q.; Zhang, T. L.; Wang, M. Y.


卷: 751; 期: 1; 页: 18-29

The propagation properties of coronal mass ejections (CMEs) are crucial to predict its geomagnetic effect. A newly developed three-dimensional (3D) mask fitting reconstruction method using coronagraph images from three viewpoints has been described and applied to the CME ejected on 2010 August 7. The CME's 3D localization, real shape, and morphological evolution are presented. Due to its interaction with the ambient solar wind, the morphology of this CME changed significantly in the early phase of evolution. Two hours after its initiation, it was expanding almost self-similarly. The CME's 3D localization is quite helpful to link remote sensing observations to in situ measurements. The investigated CME was propagating to Venus with its flank just touching STEREO B. Its corresponding interplanetary CME in the interplanetary space shows a possible signature of a magnetic cloud with a preceding shock in Venus Express (VEX) observations, while from STEREO B only a shock is observed. We have calculated three principal axes for the reconstructed 3D CME cloud. The orientation of the major axis is, in general, consistent with the orientation of a filament (polarity inversion line) observed by SDO/AIA and SDO/HMI. The flux rope axis derived by the Minimal Variance Analysis from VEX indicates a radial-directed axis orientation. It might be that locally only the leg of the flux rope passed through VEX. The height and speed profiles from the Sun to Venus are obtained. We find that the CME speed possibly had been adjusted to the speed of the ambient solar wind flow after leaving the COR2 field of view and before arriving at Venus. A southward deflection of the CME from the source region is found from the trajectory

of the CME geometric center. We attribute it to the influence of the coronal hole where the fast solar wind emanated from.

Record 30 of 193

Solar Intranetwork Magnetic Elements: Bipolar Flux Appearance

Wang, Jingxiu; Zhou, Guiping; Jin, Chunlan; Li, Hui

SOLAR PHYSICS

卷: 278; 期: 2; 页: 299-322

This study aims to quantify characteristic features of the bipolar flux appearance of solar intranetwork (IN) magnetic elements. To attack this problem, we use the Narrowband Filter Imager (NFI) magnetograms from the Solar Optical Telescope (SOT) on board Hinode; these data are from quiet and enhanced network areas. Cluster emergence of mixed polarities and IN ephemeral regions (ERs) are the most conspicuous forms of bipolar flux appearance within the network. Each of the clusters is characterized by a few well-developed ERs that are partially or fully coaligned in magnetic axis orientation. On average, the sampled IN ERs have a total maximum unsigned flux of several 10(17) Mx, a separation of 3 -aEuro parts per thousand 4 arcsec, and a lifetime of 10 -aEuro parts per thousand 15 minutes. The smallest IN ERs have a maximum unsigned flux of several 10(16) Mx, separations of less than 1 arcsec, and lifetimes as short as 5 minutes. Most IN ERs exhibit a rotation of their magnetic axis of more than 10 degrees during flux emergence. Peculiar flux appearance, e.g., bipole shrinkage followed by growth or the reverse, is not unusual. A few examples show repeated shrinkage-growth or growth-shrinkage, like magnetic floats in the dynamic photosphere. The observed bipolar behavior seems to carry rich information on magnetoconvection in the subphotospheric layer.

Record 31 of 193

A Teardrop-Shaped Ionosphere At Venus In Tenuous Solar Wind

Wei, Y.; Fraenz, M.; Dubinin, E.; Coates, A. J.; Zhang, T. L.; Wan, W.; Feng, L.; Angsmann, A.; Opitz, A.; Woch, J.; Barabash, S.; Lundin, R.

Planetary and Space Science

卷: 73; 期: 1; 页: 254-261

A very tenuous solar wind regime, following a series of large coronal mass ejections, impacted Venus during early August, 2010. STEREO-B downstream from Venus observed that the solar wind density at Earth orbit dropped to ˜0.1#/cm3 and persisted at this value over 1 day. A similar low value was observed at Earth in 1999 and has attracted comprehensive attention (Lazarus, A.J., 2000. Solar physics: the day the solar wind almost disappeared. Science 287, 2172-2173.), especially its consequences on Earth's ionosphere and magnetosphere (Lockwood, M., 2001. Astronomy: the day the solar wind nearly died. Nature 409, 677-679.).


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We now have an opportunity to examine the response of Venus' ionosphere to such a tenuous solar wind. After Venus Express spacecraft entered the ionosphere near the terminator, it continuously sampled O+ dominated planetary plasma on the nightside till it left the optical shadow region when Venus Express was located at 2 RV (Venus' Radii) to the Venus center and 1.1 RV to the Sun-Venus line. Moreover, the O+ speed was lower than the gravitational escape speed. We interpret this low-speed O+ as a constituent of the extended nightside ionosphere as a consequence of long-duration (18 h) tenuous solar wind, because the very low dynamic pressure enhances the source and reduces the sink of the nightside ionosphere. Though the full extent of the nightside ionosphere is not known due to the limitation of spacecraft's trajectory, our results suggest that the global configuration of Venus' ionosphere could resemble a teardrop-shaped cometary ionosphere.

Record 32 of 193

Unusual Emissions at Various Energies Prior to the Impulsive Phase of the Large Solar Flare and Coronal Mass Ejection of 4 November 2003

Kaufmann, Pierre; Holman, Gordon D.; Su, Yang; Guillermo Gimenez de Castro, C.; Correia, Emilia; Fernandes, Luis O. T.; de Souza, Rodney V.; Marun, Adolfo; Pereyra, Pablo

SOLAR PHYSICS

卷: 279; 期: 2; 页: 465-475

The GOES X28 flare of 4 November 2003 was the largest ever recorded in its class. It produced the first evidence for two spectrally separated emission components, one at microwaves and the other in the THz range of frequencies. We analyzed the pre-flare phase of this large flare, twenty minutes before the onset of the major impulsive burst. This period is characterized by unusual activity in X-rays, sub-THz frequencies, H alpha, and microwaves. The CME onset occurred before the onset of the large burst by about 6 min. It was preceded by pulsations of 3 -aEuro parts per thousand 5 s periods at sub-THz frequencies together with X-ray and microwave enhancements. The sub-THz pulsations faded out as impulsive bursts were detected at 100 -aEuro parts per thousand 300 keV and 7 GHz, close to the time of the first H alpha brightening and the CME onset. The activities detected prior to and at the CME onset were located nearly 2 arcmin south of the following large flare, suggesting they were separate events. This unusual activity brings new clues to understanding the complex energy buildup mechanisms prior to the CME onset, occurring at a distinct location and well before the major flare that exploded afterwards.

Record 33 of 193

Solar Magnetized "Tornadoes:" Relation to Filaments

Su, Yang; Wang, Tongjiang; Veronig, Astrid; Temmer,

Manuela; Gan, Weiqun

ASTROPHYSICAL JOURNAL LETTERS

卷: 756; 期: 2; 页: L41-L47

Solar magnetized "tornadoes," a phenomenon discovered in the solar atmosphere, appear as tornado-like structures in the corona but are rooted in the photosphere. Like other solar phenomena, solar tornadoes are a feature of magnetized plasma and therefore differ distinctly from terrestrial tornadoes. Here we report the first analysis of solar "tornadoes" (two papers which focused on different aspects of solar tornadoes were published in the Astrophysical Journal Letters and Nature, respectively, during the revision of this Letter). A detailed case study of two events indicates that they are rotating vertical magnetic structures probably driven by underlying vortex flows in the photosphere. They usually exist as a group and are related to filaments/prominences, another important solar phenomenon whose formation and eruption are still mysteries. Solar tornadoes may play a distinct role in the supply of mass and twists to filaments. These findings could lead to a new explanation of filament formation and eruption.

Record 34 of 193

Particle Acceleration and Gamma Rays in Solar Flares: Recent Observations and New Modeling

Miroshnichenko, L. I.; Gan, W. Q.

ADVANCES IN SPACE RESEARCH

卷: 50; 期: 6; 页: 736-756

Experiments on SMM, GAMMA, Yohkoh, GRAN AT, Compton GRO, INTEGRAL, RHESSI and CORONAS-F satellites over the past three decades have provided copious data for fundamental research relating to particle acceleration, transport and energetics of flares and to the ambient abundance of the solar corona, chromosphere and photosphere. We summarize main results of solar gamma-astronomy (including some results of several joint Russian-Chinese projects) and try to appraise critically a real contribution of those results into modern understanding of solar flares, particle acceleration at the Sun and some properties of the solar atmosphere. Recent findings based on the RHESSI, INTEGRAL and CORONAS-F measurements (source locations, spectrum peculiarities, He-3 abundance etc.) are especially discussed. Some unusual features of extreme solar events (e.g., 28 October 2003 and 20 January 2005) have been found in gamma-ray production and generation of relativistic particles (solar cosmic rays, or SCR). A number of different plausible assumptions are considered concerning the details of underlying physical processes during large flares: (1) existence of a steeper distribution of surrounding medium density as compared to a standard astrophysical model (HSRA) for the solar atmosphere; (2) enhanced content of the He-3 isotope; (3) formation of magnetic trap with specific properties; (4) prevailing non-uniform (e.g., fan-like) velocity (angular)


29

distributions of secondary neutrons, etc. It is emphasized that real progress in this field may be achieved only by combination of gamma-ray data in different energy ranges with multi-wave and energetic particle observations during the same event. We especially note several promising lines for the further studies: (1) resonant acceleration of the He-3 ions in the corona; (2) timing of the flare evolution by gamma-ray fluxes in energy range above 90 MeV; (3) separation of gamma-ray fluxes from different sources at/near the Sun (e.g., different acceleration sources/episodes during the same flare, contribution of energetic particles accelerated by the CME-driven shocks etc.); (4) asymmetric magnetic geometry and new magnetic topology models of the near-limb flares; (5) modeling of self-consistent time scenario of the event.

Record 35 of 193

Slowly Drifting Radio Structures in Solar Flares

Ning, Zongjun; Wu, Hongao; Xu, Fuying; Meng, Xuan

Astronomical Research & Technology

卷: 9; 期: 4; 页: 363-365

We present the data of high-frequency drift radio structures observed by the spectrometer of the Purple Mountain Observatory(PMO) over the frequency range of 4.5-7.5GHz in the solar flare of March 18,2003.Such structures have been observed to have fine features consisting of short pulses,but drift with time as a whole.The drifting structures take place before the soft X-ray maximum,almost at the maximum of hard X-ray flux of 25-50keV.For the first time,drifts toward higher frequencies are detected in this kind of radio structures near 6GHz.

Record 36 of 193

The Contraction and Shearing of Solar Flare Loops

Zhou, Tuanhui; Ji, Haisheng; Wang, Junfeng


卷: 9; 期: 4; 页: 357-362

In this paper we analyze two flares,which are the M5.7 flare of March 14,2002 and the X10 flare of October 29,2003.They both have classical two-ribbon features which were observed in TRACE UV(160.0nm) or EUV(17.1nm) images and have long-duration conjugate footpoints with hard X-ray(HXR) emission.Using the "center-of-mass" method,we find the locations of the centroids of the flare ribbons and HXR kernels.The results are as follows.(1) The conjugate ribbons in UV/EUV or kernels in HXR of the two flares show converging motions during the impulsive phase.For the two flares,the converging motions last about 3 and 10 minutes,respectively.(2) The conjugate ribbons and

footpoints of the two events exhibit strong shearing motions.The shear angles decrease during the flares.These results show that the magnetic reconnections for the flares occur in highly sheared magnetic fields.Furthermore,the results support the magnetic-field model constructed by Ji(2007),who proposed that the contraction of a flaring loop is the signature of the relaxation of sheared magnetic fields.

Record 37 of 193

Radiative and Conductive Cooling In a Solar Flare

Ning, Zongjun; Li, Dong

ASTROPHYSICS AND SPACE SCIENCE

卷: 338; 期: 1; 页: 15-21

We investigate the radiative and conductive cooling in the solar flare observed by RHESSI on 2005 September 13. The radiative and conductive loss energies are estimated from the observations after the flare onset. Consistent with previous findings, the cooling is increased with time, especially the radiation becomes remarkable on the later phase of flare. According our method, about half of thermal energy is traced by RHESSI soft X-rays, while the other half is lost by the radiative (similar to 38%) and conductive (similar to 9%) cooling at end of the hard X-rays in this event. The non-thermal energy input of P-nth (inferred from RHESSI hard X-ray spectrum) is not well correlated with the derivative of thermal energy of dE(th)/dt (required to radiate the RHESSI soft X-ray flux and spectrum) alone. However, after consideration the radiation and conduction, a high correlation is obtained between the derivative of total thermal energy (dE(th)+E-rad+E-cond/dt) and nonthermal energy input (P(nt)h) from the flare start to end, indicating the relative importance of conductive and direct radiative losses during the solar flare development. Ignoring the uncertainties to estimate the energy from the observations, we find that about similar to 12% fraction of the known energy is transferred into the thermal energy for the 2005 September 13 flare.

Record 38 of 193

Magnetic Bright Points in the Solar Atmosphere

Li, Dong; Ning, Zongjun

Progress in Astronomy

卷: 30; 期: 2; 页: 172-185

We firstly review the recent findings about the Magnetic Bright points (MBPs) on the Sun. MBPs are small-scale and short-lived structures with enhanced brightness on the solar photosphere. They have a mean diameter ranging from 100 to 300 km, and a mean lifetime of several minutes. MBPs are highly dynamic. Most of the MBPs are related to the magnetic field, especially the small-scale field in the lower solar atmosphere. MBPs are frequently observed at the region with a strong field, especially in the line of sight(LOS) strong field, i.e. up to kilogauss. Therefore,

Multi-Band Observation of Solar Activity


30

lots of magnetic energy should be stored in the MBPs. To study the MBPs is important for us to understand the progress of the radiation from the photosphere and the nature of the solar magnetic fields. Meanwhile, MBPs are thought to produce the MHD waves contributing to the coronal heating. Previous observations show that the MBPs are related to the small-scale field evolution on the photosphere, such as the coalescence of the same-polarity, the cancelation of the opposite-polarities, or the fragmentation of one magnetic field. Based on this concept, we statistically study 2722 MBPs at 1600 A from the SDO observations and the corresponding bipolar fields, and find that about 1/3 MBPs are related to the magnetic bipolar fields, indicating the cancelation of the opposite-polarities is one of the important mechanisms to produce the MBPs.

Record 39 of 193

Power Conversion Factor in Sollar Flares

Ning, ZongJun

CHINESE SCIENCE BULLETIN

卷: 57; 期: 12; 页: 1397-1404

With RHESSI data from five solar flares taken from beginning to end, we investigate the power conversion factor p defined as the ratio of the time derivative of total thermal energy (E-RHESSI + E-rad + E-cond) and the kinetic power (P-RHESSI) of nonthermal electrons. Here, E-RHESSI is the computed energy contained in thermal plasmas traced by RHESSI SXRs. Other two contributions (E-rad and E-cond) to the total energy are the energies lost through radiation and conduction, both of which can be derived from the observational data. If both are not considered, mu is only positive before the SXR maximum. However, we find that for each flare studied mu is positive over the whole duration of the soalr flare after taking into account both radiation and conduction. Mean values for mu range from 11.7% to 34.6% for these five events, indicating roughly that about this fraction of the known energy in nonthermal electrons is efficiently transformed into thermal energy from start to end. This fraction is traced by RHESSI SXR observations; the rest is lost. The bulk of the nonthermal energy could heat the plasma low in the atmosphere to drive mass flows (i.e. chromospheric evaporation).

Record 40 of 193

Observation of Ultrafine Channels of Solar Corona Heating

Ji, Haisheng; Cao, Wenda; Goode, Philip R.


卷: 570; 期: 1; 页: L25-L29

We report the first direct observations of dynamical events originating in the Sun's photosphere and subsequently lighting up the corona. Continuous small-scale, impulsive events have been tracked from

their origin in the photosphere on through to their brightening of the local corona. We achieve this by combining high-resolution ground-based data from the 1.6 m aperture New Solar Telescope (NST) at Big Bear Solar Observatory (BBSO), and satellite data from the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory (SDO). The NST imaging observations in helium I 10830 angstrom reveal unexpected complexes of ultrafine, hot magnetic loops seen to be reaching from the photosphere to the base of the corona. Most of these ultrafine loops are characterized by an apparently constant, but surprisingly narrow diameter of about 100 km all along each loop, and the loops originate on the solar surface from intense, compact magnetic field elements. The NST observations detect the signature of upward injections of hot plasma that excite the ultrafine loops from the photosphere to the base of the corona. The ejecta have their individual footpoints in the intergranular lanes between the Sun's ubiquitous, convectively driven granules. In many cases, AIA/SDO detects cospatial and cotemporal brightenings in the overlying, million degree coronal loops in conjunction with the upward injections along the ultrafine loops. Segments of some of the more intense upward injections are seen as rapid blueshifted events in simultaneous Ha blue wing images observed at BBSO. In sum, the observations unambiguously show impulsive coronal heating events from upward energy flows originating from intergranular lanes on the solar surface accompanied by cospatial mass flows.

Record 41 of 193

Frequency Dependence of the Power-Law Index of Solar Radio Bursts

Song, Qiwu; Huang, Guangli; Tan, Baolin


卷: 570; 期: 2; 页: 160-163

We process solar flare observations of Nobeyama Radio Polarimeters with an improved maximum likelihood method developed recently by Clauset et al. The method accurately extracts power-law behaviors of the peak fluxes in 486 radio bursts at six frequencies (1-35 GHz) and shows an excellent performance in this study. The power-law indices on 1-35 GHz given by this study vary around 1.74-1.87, which is consistent with earlier statistics in different solar cycles and very close to the simulations of the avalanche model by Lu.

Record 42 of 193

UV1600 Bright Points and Magnetic Bipoles in Solar Quiet Regions

Li, Dong; Ning, ZongJun


卷: 341; 期: 2; 页: 215-224

Using the observations from Atmospheric Imaging Assembly (AIA) and Helioseismic and Magnetic Imager


31

(HMI) onboard Solar Dynamics Observatory (SDO), we explore the relationship between the bright points at 1600 (1600BPs) and magnetic polarities in the quiet regions of the Sun. 1600BPs are determined from the bright regions with a brightness above the mean value of the background plus the three times of background deviation and with an area above 25 pixel(2) (9.324 arcsec(2)), while individual magnetic polarity has a strength greater than the mean value of the background plus the two and half times of background deviation and an area greater than 5 pixel(2) (1.272 arcsec(2)). And magnetic bipoles are identified as a pair of positive and negative polarities with a shortest distance between them. Based on this way, 2722 1600BPs and 2850 magnetic bipoles are identified from double square regions near disk center but symmetrically on north- and south-hemispheres respectively, with a size of 200''Au200'' each day from 19 to 25 August 2010. We find that only 29.6 % (806/2722) 1600BPs display a good correlation with magnetic bipoles, while about 64.3 % (1749/2722) 1600BPs show one-to-one correspondence to the magnetic polarities, regardless of the positive and negative polarities. For these magnetic bipoles associated with 1600BPs, we find that their orientation angles are distributed randomly along the equator.

Record 43 of 193

GRB 120422A: A Low-Luminosity Gamma-Ray Burst Driven By a Central Engine

Zhang, Bin-Bin; Fan, Yi-Zhong; Shen, Rong-Feng; Xu, Dong; Zhang, Fu-Wen; Wei, Da-Ming; Burrows, David N.; Zhang, Bing; Gehrels, Neil


卷: 756; 期: 2; 页: 190-195

GRB 120422A is a low-luminosity gamma-ray burst (GRB) associated with a bright supernova, which distinguishes itself by its relatively short T-90 (similar to 5 s) and an energetic and steep-decaying X-ray tail. We analyze the Swift Burst Alert Telescope and X-ray Telescope data and discuss the physical implications. We show that the steep decline early in the X-ray light curve can be interpreted as the curvature tail of a late emission episode around 58-86 s, with a curved instantaneous spectrum at the end of the emission episode. Together with the main activity in the first similar to 20 s and the weak emission from 40 s to 60 s, the prompt emission is variable, which points to a central engine origin in contrast to a shock-breakout origin, which is used to interpret some other nearby low-luminosity supernova GRBs. Both the curvature effect model and interpreting

the early shallow decay as the coasting external forward shock emission in a wind medium provide a constraint on the bulk Lorentz factor Gamma to be around several. Comparing the properties of GRB 120422A and other supernova GRBs, we find that the main criterion to distinguish engine-driven GRBs from shock-breakout GRBs is the time-averaged gamma-ray luminosity. Engine-driven GRBs likely have a luminosity above similar to 10(48) erg s(-1).

Record 44 of 193

Statistical Interpretation of the Spatial Distribution of Current 130 GeV Gamma-Ray Line Signal Within the Dark Matter Annihilation Scenario

Yang, Rui-Zhi; Yuan, Qiang; Feng, Lei; Fan, Yi-Zhong; Chang, Jin

PHYSICS LETTERS B

卷: 756; 期: 4-5; 页: 285-288

Recently, several groups identified a tentative gamma-ray line signal with energy similar to 130 GeV in the central Galaxy from the Fermi-EAT data. Such a gamma-ray line can be interpreted as the signal of dark matter annihilation. However, the offset similar to 220 pc (1.5 degrees) of the center of the most prominent signal region from the Galactic center Sgr A* has been thought to challenge the dark matter annihilation interpretation. Considering the fact that such a 130 GeV gamma-ray line signal consists of only similar to 14 photons, we suggest that the "imperfect" consistency of these photons with the expected dark matter distribution is due to the limited statistics. The offset will be smaller as more signal photons have been collected in the near future. Our Monte Carlo simulation supports the above speculation.

Record 45 of 193

The Photospheric Radiation Model for the Prompt Emission of Gamma-Ray Bursts: Interpreting Four Observed Correlations

Fan, Yi-Zhong; Wei, Da-Ming; Zhang, Fu-Wen; Zhang, Bin-Bin


卷: 755; 期: 1; 页: L6-L9

We show that the empirical E-p-L, Gamma-L, E-p-Gamma, and (eta) over bar (gamma)-E-p correlations (where L is the time-averaged luminosity of the prompt emission, E-p is the spectral peak energy, Gamma is the bulk Lorentz factor, and (eta) over bar (gamma) is the emission efficiency of gamma-ray bursts, GRBs) are well consistent with the relations between the analogous parameters predicted in the photospheric radiation model of the prompt emission of GRBs. The time-resolved thermal radiation of GRB 090902B does follow the E-p-L and Gamma-L correlations. A reliable interpretation of the four correlations in alternative

Laboratory for Dark Matter and Space

Astronomy


32

models is still lacking. These may point toward a photospheric origin of prompt emission of some GRBs.

Record 46 of 193

Fermi Large Area Telescope Observations of GRB 110625A

Tam, P. H. T.; Kong, A. K. H.; Fan, Yi-Zhong


卷: 754; 期: 2; 页: 117-121

Gamma-ray bursts (GRBs) that emit photons at GeV energies form a small but significant population of GRBs. However, the number of GRBs whose GeV-emitting period is simultaneously observed in X-rays remains small. We report gamma-ray observations of GRB 110625A using Fermi's Large Area Telescope in the energy range 100 MeV-20 GeV. Gamma-ray emission at these energies was clearly detected using data taken between 180 s and 580 s after the burst, an epoch after the prompt emission phase. The GeV light curve differs from a simple power-law decay, and probably consists of two emission periods. Simultaneous Swift X-Ray Telescope observations did not show flaring behaviors as in the case of GRB 100728A. We discuss the possibility that the GeV emission is the synchrotron self-Compton radiation of underlying ultraviolet flares.

Record 47 of 193

Deep observation of the giant radio lobes of Centaurus A with the Fermi Large Area Telescope

Yang, R. -Z.; Sahakyan, N.; Wilhelmi, E. de Ona; Aharonian, F.; Rieger, F.


卷: 542; 页: A19-A26

The detection of high-energy (HE) gamma-ray emission up to similar to 3 GeV from the giant lobes of the radio galaxy Centaurus A has been recently reported by the Fermi-LAT Collaboration based on ten months of all-sky survey observations. A data set more than three times larger is used here to study the morphology and photon spectrum of the lobes with higher statistics. The larger data set results in the detection of HE gamma-ray emission (up to similar to 6 GeV) from the lobes with a significance of more than 10 and 20 sigma for the north and the south lobe, respectively. Based on a detailed spatial analysis and comparison with the associated radio lobes, we report evidence for a substantial extension of the HE gamma-ray emission beyond the WMAP radio image for the northern lobe of Cen A. We reconstructed the spectral energy distribution (SED) of the lobes using radio (WMAP) and Fermi-LAT data from the same integration region. The implications are discussed in the context of hadronic and time-dependent leptonic scenarios.

Record 48 of 193

Estimating The Background Count Rate in the Energy Field From 0.55-2.75 MeV for Chang'E-1 Gamma-Ray Spectrometer

Ma, T.; Chang, J.; Zhang, N.; Wu, J.

NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A

卷: 664; 期: 1; 页: 232-235

With a large geometrical area, the Gamma-ray spectrometer (GRS) onboard Chang'E-1 was designed to detect gamma rays from the moon. The scientific objective is to study the element information including both type and abundance by distinguishing the energy of gamma ray peak relative to elements and calculating the peak area counts. Regretfully, the cislunar spectrum of GRS was not collected. Nevertheless, we give a method to estimate the background count rate in the energy field from 0.55-2.75 MeV. A natural radioactivity count rate map in 2 degrees x 2 degrees grids is shown after reducing the background count rate and the uncertainty of the result is discussed.

Record 49 of 193

GRB 081029: A Gamma-Ray Burst with A Multi-Component Afterglow

Holland, Stephen T.; De Pasquale, Massimiliano; Mao, Jirong; Sakamoto, Takanori; Schady, Patricia; Covino, Stefano; Fan, Yi-Zhong; Jin, Zhi-Ping; D'Avanzo, Paolo; Antonelli, Angelo; D'Elia, Valerio; Chincarini, Guido; Fiore, Fabrizio; Pandey, Shashi Bhushan; Cobb, Bethany E.


卷: 745; 期: 1; 页: 41-52

We present an analysis of the unusual optical light curve of the gamma-ray burst GRB 081029, a long-soft burst with a redshift of z = 3.8479. We combine X-ray and optical observations from the Swift X-Ray Telescope and the Swift UltraViolet/Optical Telescope with ground-based optical and infrared data obtained using the REM, ROTSE, and CTIO 1.3 m telescopes to construct a detailed data set extending from 86 s to similar to 100000 s after the BAT trigger. Our data cover a wide energy range from 10 keV to 0.77 eV (1.24 angstrom-16000 angstrom). The X-ray afterglow shows a shallow initial decay followed by a rapid decay starting at about 18000 s. The optical and infrared afterglow, however, shows an uncharacteristic rise at about 3000 s that does not correspond to any feature in the X-ray light curve. Our data are not consistent with synchrotron radiation from a jet interacting with an external medium, a two-component jet, or continuous energy injection from the central engine. We find that the optical light curves can be broadly explained by a collision between two ejecta shells within a two-component jet. A growing number of gamma-ray-burst afterglows are consistent with complex jets, which suggests that some (or all)


33

gamma-ray-burst jets are complex and will require detailed modeling to fully understand them.

Record 50 of 193

Dark Matter Mini-Halo around the Compact Objects: The Formation, Evolution and Possible Contribution to the Cosmic Ray Electrons/Positrons

Yang, Rui-Zhi; Fan, Yi-Zhong; Waldman, Roni; Chang, Jin

JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS

卷: 2012; 期: 01; 页: 023-034

Dark matter particles may be captured by a star and then thermalized in the star's core. At the end of its life a massive star collapses suddenly and a compact object is formed. The dark matter particles redistribute accordingly. In the inelastic dark matter model, an extended dense dark matter mini-halo surrounding the neutron star may be formed. Such mini-halos may be common in the Galaxy. The electron/positron flux resulting in the annihilation of dark matter particles, however, is unable to give rise to observable signal unless a nascent mini-halo is within a distance similar to a few 0.1 pc from the Earth.

Record 51 of 193

A High Dynamic Range Readout Unit for a Calorimeter

Zhang Yun-Long; Li Bing; Feng Chang-Qing; Li Xian-Li; Wang Xiao-Lian; Xu Zi-Zong; Guo Jian-Hua; Cai Ming-Sheng; Hu Yi-Ming; Wu Jian; Chang Jin

CHINESE PHYSICS C

卷: 36; 期: 1; 页: 71-73

A high dynamic range readout system, consisting of a multi-dynode readout PMT and a VA32 chip, is presented. An LED system is set up to calibrate the relative gains between the dynodes, and the ADC counts per MIPs from dynode 7 are determined under cosmic-ray calibration. A dynamic range from 0.5 MIPs to 1 x 10(5) MIPs is achieved.

Record 52 of 193

CHANDRA/HETGS Observations of the Brightest Flare Seen From Sgr A*

Nowak, M. A.; Neilsen, J.; Markoff, S. B.; Baganoff, F. K.; Porquet, D.; Grosso, N.; Levin, Y.; Houck, J.; Eckart, A.; Falcke, H.; Ji, L.; Miller, J. M.; Wang, Q. D.


卷: 759; 期: 2; 页: 95-103

Starting in 2012, we began an unprecedented observational program focused on the supermassive black hole in the center of our Galaxy, Sgr A*, utilizing the High Energy Transmission Grating Spectrometer (HETGS) instrument on the Chandra X-Ray Observatory. These observations will allow us to measure the

quiescent X-ray spectra of Sgr A* for the first time at both high spatial and spectral resolution. The X-ray emission of Sgr A*, however, is known to flare roughly daily by factors of a few to ten times over quiescent emission levels, with rarer flares extending to factors of greater than 100 times quiescence. Here we report an observation performed on 2012 February 9 wherein we detected what are the highest peak flux and fluence flare ever observed from Sgr A*. The flare, which lasted for 5.6 ks and had a decidedly asymmetric profile with a faster decline than rise, achieved a mean absorbed 2-8 keV flux of (8.5 +/- 0.9) x 10(-12) erg cm(-2) s(-1). The peak flux was 2.5 times higher, and the total 2-10 keV emission of the event was approximately 10(39) erg. Only one other flare of comparable magnitude, but shorter duration, has been observed in Sgr A* by XMM-Newton in 2002 October. We perform spectral fits of this Chandra-observed flare and compare our results to the two brightest flares ever observed with XMM-Newton. We find good agreement among the fitted spectral slopes (Gamma similar to 2) and X-ray absorbing columns (N-H similar to 15 x 10(22) cm(-2)) for all three of these events, resolving prior differences (which are most likely due to the combined effects of pileup and spectral modeling) among Chandra and XMM-Newton observations of Sgr A* flares. We also discuss fits to the quiescent spectra of Sgr A*.

Record 53 of 193

Readout Electronics Design of prototype of BGO Calorimeter in Chinese Space Detector for Dark Matter Particle

Guo, Jianhua; Cai, Mingsheng; Hu, Yiming; Chang, Jin


卷: 53; 期: 1; 页: 72-79

The goal of the space detector for dark matter,which is proposed by Purple Mountain Observatory of Chinese Academy of Sciences,is to measure the energy spectra of the gamma-rays and electrons.The whole detector consists of BGO calorimeter and scintillator hodoscope.The detector has a capability of measuring the particles energy in 10 GeV to 10 TeV,and the main energy of injected particle is deposited in the BGO calorimeter. This paper will introduce the prototype of readout electronics of BGO calorimeter.

Record 54 of 193

Development of the DAQ System of Chinese High Energy Cosmic Ray Detector in Space

Guo jianhua; Xu, Zunlei; Cai Mingsheng; Hu, yiming; Ghang, Jin

32nd international cosmic ray conference

卷: 5; 页: 252-253

The main purpose of the Chinese high energy cosmic ray detector in space is to measure the energy


34

spectrum of high energy electron and gamma ray. The energy range of the detector is about 50GeV-10TeV. The detector consists of BGO calorimeter and scintillation hodoscope. This paper will introduce the data acquisition system (DAQ) of the whole detector, which packages the data from the calorimeter and hodoscope and sends it to the mass memory in the satellite.

Record 55 of 193

Expected Performance of the Chinese High Energy Cosmic Particle Detector to Be In Space

Wu, J.; Chang, J.


卷: 5; 页: 228-231

This paper presents simulation results for basic operation of the first Chinese high energy cosmic particle detector aiming to detect electron/gamma at the range between 10GeV and 10TeV in space. The new detector is described with its characteristics of good energy and space resolution and strong separation power for electron and proton. A GEANT4 code has been used for a dynamic simulation of the detector. The detector structure is illustrated and results of simulating electron/proton/gamma incidence on the detector validate its operation.

Record 56 of 193

Study of Backward-Propagating Langmuir Waves with Numerical Simulations Based on the Particle-in-Cell Method

Huang, Yu; Huang Guangli


卷: 9; 期: 4; 页: 353-356

The conversion of Langmuir waves into electromagnetic

radiations is an important mechanism of Type Ⅲ solar

bursts.Langmuir Waves(LW) can be easily excited by electron-beam instabilities,and they can become backward propagating throuth the wave-wave interaction.Generally,the backward-propagating LW are very important for the second-harmonic waves of Type

Ⅲ solar bursts.In this paper we pay particular attention to the mechanism of the backward-propagating LW as revealed through numerical simulations based on the Partical-in-Cell(PIC) method.We found that ions play a key role to excite the backward-propagating LW,with draw much of their energy from the scattering of the forward-propagating LW.Moreover,an electron beam can hardly generate backward-propagating LW directly,but may directly amplify second-harmonic forward-propagating LW.

Record 57 of 193

Ejected-Electron Spectroscopy of Autoionizing Resonances of Helium Excited By Fast-Electron Impact

Zhang, Zhe; Shan, Xu; Wang, Enliang; Chen, Xiangjun

Physical Review A

卷: 86; 期: 6; 页: 062702-1-062702-8

The autoionizing resonances (2s2)1S, (2p2)1D, and (2s2p)1P of helium have been investigated employing ejected-electron spectroscopy by fast-electron impact at incident energies of 250-2000 eV and ejected angles of 26°-116°. Shore parameters of the line shapes for these three resonances have been obtained in such high incident energy regime except at 250 eV. Distinct discrepancies between the present results at 250 eV and those of McDonald and Crowe at 200 eV [D. G. McDonald and A. Crowe, J. Phys. BJPAMA40953-407510.1088/0953-4075/25/9/018 25, 2129 (1992); D. G. McDonald and A. Crowe, J. Phys. BJPAMA40953-407510.1088/0953-4075/25/20/024 25, 4313 (1992)] and Sise at 250 eV [O. Sise, M. Dogan, I. Okur, and A. Crowe, Phys. Rev. APLRAAN1050-294710.1103/PhysRevA.84.022705 84, 022705 (2011)], especially for 1D and 1P states, are also observed.

Record 58 of 193

Mechanical Design of BGO Calorimeter for Chinese High Energy Cosmic Ray Detector in Space

Yiming, Hu


卷: 5; 页: 254-256

The BGO calorimeter is the main component of the Chinese high energy cosmic ray detector. The BGO calorimeter consists of 576 BGO Crystals coupled with photomultiplier tube. The reliability and safety of the BGO Calorimeter structure play a very important role in the operation of whole detector. During the rocket launch, the calorimeter structure should be stable against vibration and environmental factors to ensure the detector works in good conditions. In this article, we make the BGO calorimeter structure design, and then prove that it will work in the environments of rocket launch and flight.


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II. Antarctic Astronomy Radio Astronomy

Record 59 of 193

Sound-Speed Inversion of the Sun Using a Nonlocal Statistical Convection Theory

Zhang, Chunguang; Deng, Licai; Xiong, Darun; Christensen-Dalsgaard, Jorgen


卷: 759; 期: 1; 页: L14-L18

Helioseismic inversions reveal a major discrepancy in sound speed between the Sun and the standard solar model just below the base of the solar convection zone. We demonstrate that this discrepancy is caused by the inherent shortcomings of the local mixing-length theory adopted in the standard solar model. Using a self-consistent nonlocal convection theory, we construct an envelope model of the Sun for sound-speed inversion. Our solar model has a very smooth transition from the convective envelope to the radiative interior, and the convective energy flux changes sign crossing the boundaries of the convection zone. It shows evident improvement over the standard solar model, with a significant reduction in the discrepancy in sound speed between the Sun and local convection models.

Record 60 of 193

Status of the First Antarctic Survey Telescopes for Dome A

Zhengyang Li ; Xiangyan Yuan ; Xiangqun Cui ; Daxing Wang ; Xuefei Gong ; Fujia Du ; Yi Zhang ; Yi Hu ; Haikun Wen ; Xiaoyan Li ; Lingzhe Xu ; Zhaohui Shang ; Wang, Lifan

Proceedings of SPIE - The International Society for Optical Engineering

卷: 8444; 期: 1; 页: 84441O-1-84441O-7

The preliminary site testing carried out since the beginning of 2008 shows the Antarctic Dome A is very likely to be the best astronomical site on earth even better than Dome C and suitable for observations

ranging from optical wavelength to infrared and sub-millimeter. After the Chinese Small Telescope Array (CSTAR) which is composed of four small fixed telescopes with diameter of 145mm and mounted on Dome A in 2008 for site testing and variable star monitor, three Antarctic Survey Telescopes (AST3) were proposed for observations of supernovas and extrasolar planets searching. AST3 is composed of 3 large field of view catadioptric telescopes with 500mm entrance diameter and G, R, I filter for each. The telescopes can point and track autonomously along with a light and foldable dome to keep the snow and icing build up. A precise auto-focusing mechanism is designed to make the telescope work at the right focus under large temperature difference. The control and tracking components and assembly were successfully tested at from normal temperature down to -80 Celsius degree. Testing observations of the first AST3 showed it can deliver good and uniform images over the field of 8 square degrees. The first telescope was successfully mounted on Dome A in Jan. 2012 and the automatic observations were started from Mar. 2012.

Record 61 of 193

Operation, Control, and Data System for Antarctic Survey Telescope (AST3)

Shang, Zhaohui; Hu, Keliang; Hu, Yi; Li, Jiliang; Li, Jin; Liu, Qiang; Ma, Bin; Quinn, Jason L.; Sun, Jizhou; Wang, Lifan; Xiao, Jian; Yu, Jia; Yu, Ce; Yang, Mujin; Yuan, Xiangyan; Zeng, Zhen

Observatory Operations: Strategies, Processes, and Systems IV. Proceedings of the SPIE

卷: 8448; 页: 844826-1-844826-7

The first of the trio Antarctic Survey Telescopes (AST3) has been deployed to Dome A, Antarctica in January 2012. This largest optical survey telescope in Antarctica is equipped with a 10k × 10k CCD. The huge amount of data, limited satellite communication bandwidth, low temperature, low pressure and limited energy supply all place challenges to the control and operation of the telescope. We have developed both the hardware and software systems to operate the unattended telescope and carry out the survey automatically. Our systems include the main survey control, data storage, real-time pipeline, and database, for all of which we have dealt with various technical difficulties. These include developing customized computer systems and data storage arrays working at the harsh environment, temperature control for the disk arrays, automatic and fast data reduction in real-time, and building robust

Center for Antarctic Astronomy

Stellar Structure, Evolution and Pulsation


36

database system.

Record 62 of 193

Bulk Flow of Halos in Lambda CDM Simulation

Li, Ming; Jun Pan; Liang Gao; Yipeng Jin; Xiaohu Yang; Xuebin Chi; Longlong Feng; Xi Kang; Weipeng Lin; Guihua Shan; Long Wang; Donghai Zhao; Pengjie Zhang

The Astrophysical Journal

卷: 761; 期: 2; 页: 151-161

Analysis of the Pangu N-body simulation validates that the bulk flow of halos follows a Maxwellian distribution with variance that is consistent with the prediction of the linear theory of structure formation. We propose that the consistency between the observed bulk velocity and theories should be examined at the effective scale of the radius of a spherical top-hat window function yielding the same smoothed velocity variance in linear theory as the sample window function does. We compared some recently estimated bulk flows from observational samples with the prediction of the ΛCDM model we used; some results deviate from expectation at a level of ∼3σ, but the discrepancy is not as severe as previously claimed. We show that bulk flow is only weakly correlated with the dipole of the internal mass distribution, that the alignment angle between the mass dipole and the bulk flow has a broad distribution peaked at ∼30°-50°, and also that the bulk flow shows little dependence on the mass of the halos used in the estimation. In a simulation of box size 1 h–1 Gpc, for a cell of radius 100 h–1 Mpc the maximal bulk velocity is >500 km s–1; dipoles of the environmental mass outside the cell are not tightly aligned with the bulk flow, but are rather located randomly around it with separation angles ∼20°-40°. In the fastest cell there is a slightly smaller number of low-mass halos; however, halos inside are clustered more strongly at scales ≳ 20 h–1 Mpc, which might be a significant feature since the correlation between bulk flow and halo clustering actually increases in significance beyond such scales.

Record 63 of 193

The Dynamical State and Mass-Concentration Relation of Galaxy Clusters

Ludlow, Aaron D.; Navarro, Julio F.; Li, Ming; Angulo, Raul E.; Boylan-Kolchin, Michael; Bett, Philip E.


卷: 427; 期: 2; 页: 1322-1328

We use the Millennium Simulation series to study how the dynamical state of dark matter haloes affects the relation between mass and concentration. We find that a large fraction of massive systems are identified when they are substantially out of equilibrium and in a particular phase of their dynamical evolution: the more

massive the halo, the more likely it is found at a transient stage of high concentration. This state reflects the recent assembly of massive haloes and corresponds to the first pericentric passage of recently accreted material when, before virialization, the kinetic and potential energies reach maximum and minimum values, respectively. This result explains the puzzling upturn in the mass-concentration relation reported in recent work for massive haloes; indeed, the upturn disappears when only dynamically relaxed systems are considered in the analysis. Our results warn against applying simple equilibrium models to describe the structure of rare, massive galaxy clusters and urge caution when extrapolating scaling laws calibrated on lower mass systems, where such deviations from equilibrium are less common. The evolving dynamical state of galaxy clusters ought to be carefully taken into account if cluster studies are to provide precise cosmological constraints.

Record 64 of 193

Precipitable Water Vapor above Dome A, Antarctica, Determined From Diffuse Optical Sky Spectra

Sims, Geoff; Ashley, Michael C. B.; Cui, Xiangqun; Everett, Jon R.; Feng, LongLong; Gong, Xuefei; Hengst, Shane; Hu, Zhongwen; Kulesa, Craig; Lawrence, Jon S.; Luong-Van, Daniel M.; Ricaud, Philippe; Shang, Zhaohui; Storey, John W. V.; Wang, Lifan; Yang, Huigen; Yang, Ji; Zhou, Xu; Zhu, Zhenxi

PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC

卷: 124; 期: 911; 页: 74-83

The high altitudes and extremely low temperatures of the Antarctic plateau result in an exceedingly low atmospheric water vapor content. In this article we estimate the precipitable water vapor at Dome A using optical spectra of the diffuse solar irradiance in the zenith direction. The spectra were obtained from the Nigel spectrometer at Dome A during 2009. We find that the Nigel spectra contain sufficient information to extract daily average water vapor estimates, which agree with satellite observations to within +/- 0.22 mm. Finally, we use these water vapor estimates to model the optical and near-IR transmission (between 700 nm and 2.5 mu m) of Dome A to demonstrate significant advantages gained in this wavelength range and compare it with that of Paranal and Chajnantor, two midlatitude observatories.

Record 65 of 193

Physical Origin of Multi-Wavelength Emission of GRB 100418A and Implications for Its Progenitor

Jia, Lan-Wei; Wu, Xue-Feng; Lu, Hou-Jun; Hou, Shu-Jin; Liang, En-Wei


卷: 12; 期: 4; 页: 411-418


37

Swift GRB 100418A is a long burst at z = 0.624 without detection of any associated supernova (SN). Its light curves in both the prompt and afterglow phases are similar to GRB 060614, a nearby long GRB without an associated SN. We analyze the observational data of this event and discuss the possible origins of its multi-wavelength emission. We show that its joint light curve at 1 keV derived from Swift BAT and XRT observations is composed of two distinguished components. The first component, whose spectrum is extremely soft (Gamma = 4.32), ends with a steep decay segment, indicating the internal origin of this component. The second component is a slowly-rising, broad bump which peaks at similar to 10(5) s post the BAT trigger. Assuming that the late bump is due to onset of the afterglow, we derive the initial Lorentz factor (Gamma(0)) of the GRB fireball and find that it significantly deviates from the relation between the Gamma(0) and isotropic gamma-ray energy derived from typical GRBs. We also check whether it follows the same anti-correlation between X-ray luminosity and the break time observed in the shallow decay phase of many typical GRBs, which is usually regarded as a signal of late energy injection from the GRB central engine. However, we find that it does not obey this correlation. We propose that the late bump could be contributed by a two-component jet. We fit the second component with an off-axis jet model for a constant medium density and find the late bump can be represented by the model. The derived jet half-opening angle is 0.30 rad and the viewing angle is 0.315 rad. The medium density is 0.05 cm(-3), possibly suggesting that it may be from a merger of compact stars. The similarity between GRBs 060614 and 100418A may indicate that the two GRBs are from the same population and the late bump observed in the two GRBs may be a signal of a two-component jet powered by the GRB central engine.

Record 66 of 193

Modeling Photodisintegration-Induced TeV Photon Emission from Low-Luminosity Gamma-Ray Bursts

Liu, Xue-Wen; Wu, Xue-Feng; Lu, Tan

ASTRONOMICAL JOURNAL

卷: 143; 期: 5; 页: 115-118

Ultra-high-energy cosmic-ray heavy nuclei have recently been considered as originating from nearby low-luminosity gamma-ray bursts that are associated with Type Ibc supernovae. Unlike the power-law decay in long duration gamma-ray bursts, the light curve of these bursts exhibits complex UV/optical behavior: shock breakout dominated thermal radiation peaks at about 1 day, and, after that, nearly constant emission sustained by radioactive materials for tens of days. We show that the highly boosted heavy nuclei at PeV energy interacting with the UV/optical photon field will produce considerable TeV photons via the photodisintegration/photo-de-excitation process. It was later predicted that a thermal-like gamma-ray spectrum

peaks at about a few TeV, which may serve as evidence of nucleus acceleration. The future observations by the space telescope Fermi and by the ground atmospheric Cherenkov telescopes such as H. E. S. S., VERITAS, and MAGIC will shed light on this prediction.

Record 67 of 193

Panchromatic Observations of the Textbook GRB 110205a: Constraining Physical Mechanisms of Prompt Emission and Afterglow

Zheng, W.; Shen, R. F.; Sakamoto, T.; Beardmore, A. P.; De Pasquale, M.; Wu, X. F.; Gorosabel, J.; Urata, Y.; Sugita, S.; Zhang, B.; Pozanenko, A.; Nissinen, M.; Sahu, D. K.; Im, M.; Ukwatta, T. N.; Andreev, M.; Klunko, E.; Volnova, A.; Akerlof, C. W.; Anto, P.; Barthelmy, S. D.; Breeveld, A.; Carsenty, U.; Castillo-Carrion, S.; Castro-Tirado, A. J.; Chester, M. M.; Chuang, C. J.; Cunniffe, R.; Postigo, A. De Ugarte; Duffard, R.; Flewelling, H.; Gehrels, N.; Guever, T.; Guziy, S.; Hentunen, V. P.; Huang, K. Y.; Jelinek, M.; Koch, T. S.; Kubanek, P.; Kuin, P.; McKay, T. A.; Mottola, S.; Oates, S. R.; O'Brien, P.; Ohno, M.; Page, M. J.; Pandey, S. B.; Perez del Pulgar, C.; Rujopakarn, W.; Rykoff, E.; Salmi, T.; Sanchez-Ramirez, R.; Schaefer, B. E.; Sergeev, A.; Sonbas, E.; Sota, A.; Tello, J. C.; Yamaoka, K.; Yost, S. A.; Yuan, F.


卷: 751; 期: 2; 页: 90-110

We present a comprehensive analysis of a bright, long-duration (T-90 similar to 257 s) GRB 110205A at redshift z = 2.22. The optical prompt emission was detected by Swift/UVOT, ROTSE-IIIb, and BOOTES telescopes when the gamma-ray burst (GRB) was still radiating in the gamma-ray band, with optical light curve showing correlation with gamma-ray data. Nearly 200 s of observations were obtained simultaneously from optical, X-ray, to gamma-ray (1 eV to 5 MeV), which makes it one of the exceptional cases to study the broadband spectral energy distribution during the prompt emission phase. In particular, we clearly identify, for the first time, an interesting two-break energy spectrum, roughly consistent with the standard synchrotron emission model in the fast cooling regime. Shortly after prompt emission (similar to 1100 s), a bright (R = 14.0) optical emission hump with very steep rise (alpha similar to 5.5) was observed, which we interpret as the reverse shock (RS) emission. It is the first time that the rising phase of an RS component has been closely observed. The full optical and X-ray afterglow light curves can be interpreted within the standard reverse shock (RS) + forward shock (FS) model. In general, the high-quality prompt and afterglow data allow us to apply the standard fireball model to extract valuable information, including the radiation mechanism (synchrotron), radius of prompt emission (R-GRB similar to 3 x 10(13) cm), initial Lorentz factor of the outflow (Gamma(0) similar to 250), the composition of the ejecta (mildly magnetized), the collimation angle, and the total energy budget.


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Record 68 of 193

Airglow and Aurorae at Dome A, Antarctica

Sims, Geoff; Ashley, Michael C. B.; Cui, Xiangqun; Everett, Jon R.; Feng, LongLong; Gong, Xuefei; Hengst, Shane; Hu, Zhongwen; Lawrence, Jon S.; Luong-Van, Daniel M.; Moore, Anna M.; Riddle, Reed; Shang, Zhaohui; Storey, John W. V.; Tothill, Nick; Travouillon, Tony; Wang, Lifan; Yang, Huigen; Yang, Ji; Zhou, Xu; Zhu, Zhenxi

PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC

卷: 124; 期: 916; 页: 637-649

Despite the absence of artificial light pollution at Antarctic plateau sites such as Dome A, other factors such as airglow, aurorae, and extended periods of twilight have the potential to adversely affect optical observations. We present a statistical analysis of the airglow and aurorae at Dome A using spectroscopic data from Nigel, an optical/near-IR spectrometer operating in the 300-850 nm range. These data complement photometric images from Gattini, a wide-field (90 degrees) CCD camera with B, V, and R filters, allowing the background sky brightness to be disentangled from the various airglow and auroral emission lines. The median auroral contribution to the B, V, and R photometric bands is found to be 22.9, 23.4, and 23.0 mag arcsec(-2), respectively. Auroral emissions most frequently occur between 10-23 hr local time, when up to 50% of observations are above airglow-level intensities. While infrequent, the strongest emissions detected occurred in the hours just prior to magnetic midnight. We are also able to quantify the amount of annual dark time available as a function of wavelength, as well as in the standard BV R photometric bands. On average, twilight ends when the Sun reaches a zenith distance of 102.6 degrees.

Record 69 of 193

GRB 110721A: Photosphere "Death Line" And the Physical Origin of the GRB Band Function

Zhang, Bing; Lu, Rui-Jing; Liang, En-Wei; Wu, Xue-Feng


卷: 758; 期: 2; 页: L34-L38

The prompt emission spectra of gamma-ray bursts (GRBs) usually have a dominant component that is well described by a phenomenological Band function. The physical origin of this spectral component is debated. Although the traditional interpretation is synchrotron radiation of non-thermal electrons accelerated in internal shocks or magnetic dissipation regions, the growing trend within the community is to interpret this component as modified thermal emission from a

dissipative photosphere of a GRB fireball. We analyze the time-dependent spectrum of GRB 110721A detected by the Fermi Gamma-Ray Burst Monitor and Large Area Telescope, and pay special attention to the rapid evolution of the peak energy E-p. We define a "death line" of thermally dominated dissipative photospheric emission in the E-p-L plane, and show that E-p of GRB 110721A at the earliest epoch has a very high E-p similar to 15MeV that is beyond the "death line." Together with the finding that an additional "shoulder" component exists in this burst that is consistent with a photospheric origin, we suggest that at least for some bursts, the Band component is not from a dissipative photosphere, but must invoke a non-thermal origin (e.g., synchrotron or inverse Compton) in the optically thin region of a GRB outflow. We also suggest that the rapid hard-to-soft spectral evolution is consistent with the quick discharge of magnetic energy in a magnetically dominated outflow in the optically thin region.

Record 70 of 193

Exploring Galaxy Formation Models and Cosmologies with Galaxy Clustering

Kang, X.; Li, M.; Lin, W. P.; Elahi, P. J.


卷: 422; 期: 1; 页: 804-811

Using N-body simulations and galaxy formation models, we study the galaxy stellar mass correlation and the two-point autocorrelation. The simulations are run with cosmological parameters from the Wilkinson Microwave Anisotropy Probe (WMAP) first-, third-and seven-year results, which mainly differ in the perturbation amplitude of sigma(8). The stellar mass of galaxies is determined using either a semi-analytical galaxy formation model or a simple empirical abundance matching method. Compared to the Sloan Digital Sky Survey (SDSS) DR7 data at z = 0 and the DEEP2 results at z = 1, we find that the predicted galaxy clusterings from the semi-analytical model are higher than the data at small scales, regardless of the adopted cosmology. Conversely, the abundance matching method predicts good agreement with the data at both z = 0 and z = 1 for high-sigma(8) cosmologies (WMAP1 and WMAP7), but the predictions from a low-sigma(8) cosmology (WMAP3) are significantly lower than the data at z = 0. We find that the excess clustering at small scales in the semi-analytical model mainly arises from satellites in massive haloes, indicating that either the star formation is too efficient in low-mass haloes or tidal stripping is too inefficient at high redshift. Our results show that galaxy clustering is strongly affected

Galaxy Cosmology and Dark Energy


39

by the models for galaxy formation, and thus can be used to constrain the baryonic physics. The weak dependence of galaxy clustering on cosmological parameters makes it difficult to constrain the WMAP1 and WMAP7 cosmologies.

Record 71 of 193

Little Things

Hunter, Deidre A.; Ficut-Vicas, Dana; Ashley, Trisha; Brinks, Elias; Cigan, Phil; Elmegreen, Bruce G.; Heesen, Volker; Herrmann, Kimberly A.; Johnson, Megan; Oh, Se-Heon; Rupen, Michael P.; Schruba, Andreas; Simpson, Caroline E.; Walter, Fabian; Westpfahl, David J.; Young, Lisa M.; Zhang, Hong-Xin


卷: 144; 期: 5; 页: 134-162

We present LITTLE THINGS (Local Irregulars That Trace Luminosity Extremes, The Hi Nearby Galaxy Survey), which is aimed at determining what drives star formation in dwarf galaxies. This is a multi-wavelength survey of 37 dwarf irregular and 4 blue compact dwarf galaxies that is centered around Hi-line data obtained with the National Radio Astronomy Observatory (NRAO) Very Large Array (VLA). The Hi-line data are characterized by high sensitivity (<= 1.1 mJy beam(-1) per channel), high spectral resolution (<= 2.6 km s(-1)), and high angular resolution (similar to 6 ''). The LITTLE THINGS sample contains dwarf galaxies that are relatively nearby (<= 10.3 Mpc; 6 '' is <= 300 pc), that were known to contain atomic hydrogen, the fuel for star formation, and that cover a large range in dwarf galactic properties. We describe our VLA data acquisition, calibration, and mapping procedures, as well as Hi map characteristics, and show channel maps, moment maps, velocity-flux profiles, and surface gas density profiles. In addition to the Hi data we have GALEX UV and ground-based UBV and H alpha images for most of the galaxies, and JHK images for some. Spitzer mid-IR images are available for many of the galaxies as well. These data sets are available online.

Record 72 of 193

Some Updates on the Star Formation Laws in Galaxies

Gao, Yu

AAS Meeting

卷: 220; 期: 308; 页: 04-05

We highlight some of our recent studies on the global star formationlaws in galaxies. 1) We show that the surface density of dense molecular gas (traced by HCN) has the tightest linear correlation with that ofstar formation rate (SFR). There is no unique slope between the surface densities of SFR and total gas, using a large

sample of over 150galaxies including (ultra)luminous IR galaxies [(U)LIRGs]. The correlation slopes change from 1 for normal spirals to 1.5 when more and more (U)LIRGs are included. 2) Our observations using other dense gas tracer like CS further reveal that the SFR and dense gas relationship is linearly in all galaxies observed so far. 3) The locally resolved SFR-HCN correlation in M51 or the local star formation law in dense gas is also consistent with the globally established linear SFR-HCN correlation. These suggest that SFR depends linearly upon the mass of dense molecular gas. This is different from the traditional Kennicutt-Schmidt law that relates the total gas and SFR, which has no unique power-law slope.

Record 73 of 193

High Resolution SMA Imaging of (Ultra)-Luminous Infrared Galaxies

Tan, Qinghua; Gao, Yu; Wang, Zhong; U, Vivian

The Spectral Energy Distribution of Galaxies, Proceedings of the International Astronomical Union, IAU Symposium

卷: 284; 页: 471-474

We present preliminary results on Submillimeter Array (SMA) observations of three Luminous Infrared Galaxies (LIRGs) and one infrared Quasi Stellar Object (IR QSO). The galaxies were observed at sub-kpc spatial resolution in lines of CO and 13CO, as well as in the continuum at 1.3mm. The moment maps show that the molecular gas in these galaxies is distributed in rotating disks with velocity gradients ranging from ~30 to 120 km s-1 kpc-1. Combined with archival CO J=3-2 data, the spatial distributions of the CO J=3-2/J=2-1 ratios shows clear variations across the galaxies. The brightness temperature of the overlap region in VV 114 is found to be lower than that in the nuclear region of VV 114E, suggesting that that the bulk of molecular gas in this region is sub-thermalized.

Record 74 of 193

The Molecular Gas in Luminous Infrared Galaxies - I. CO Lines, Extreme Physical Conditions and Their Drivers

Papadopoulos, Padelis P.; van der Werf, Paul P.; Xilouris, E. M.; Isaak, K. G.; Gao, Yu; Muehle, S.


卷: 426; 期: 4; 页: 2601-2629

We report results from a large molecular line survey of luminous infrared galaxies (L(IR) greater than or similar to 10(11) L(circle dot)) in the local Universe (z less than or similar to 0.1), conducted during the last decade with the James Clerk Maxwell Telescope and the IRAM 30-m telescope. This work presents the CO and 13CO line data for 36 galaxies, further augmented by multi-J total CO line luminosities available for other infrared (IR) bright galaxies from the literature. This yields a

Star Formation in Galaxies


40

combined sample of N = 70 galaxies with the star formation (SF) powered fraction of their IR luminosities spanning L(IR)((+))similar to(10(10)-2 x10(12))L(circle dot) and a wide range of morphologies. Simple comparisons of their available CO spectral line energy distributions (SLEDs) with local ones, as well as radiative transfer models, discern a surprisingly wide range of average interstellar medium (ISM) conditions, with most of the surprises found in the high-excitation regime. These take the form of global CO SLEDs dominated by a very warm (T(kin) greater than or similar to 100 K) and dense (n >= 10(4) cm(-3)) gas phase, involving galaxy-sized (similar to(few) x 10(9) M(circle dot)) gas mass reservoirs under conditions that are typically found only for similar to(13) per cent of mass per typical SF molecular cloud in the Galaxy. Furthermore, some of the highest excitation CO SLEDs are found in ultraluminous infrared galaxies (ULIRGs; L(IR) >= 10(12)L(circle dot)) and surpass even those found solely in compact SF-powered hot spots in Galactic molecular clouds. Strong supersonic turbulence and high cosmic ray energy densities rather than far-ultraviolet/optical photons or supernova remnant induced shocks from individual SF sites can globally warm the large amounts of dense gas found in these merger-driven starbursts and easily power their extraordinary CO line excitation. This exciting possibility can now be systematically investigated with Herschel and the Atacama Large Milimeter Array (ALMA). As expected for an IR-selected (and thus SF rate selected) galaxy sample, only few cold CO SLEDs are found, and for fewer still a cold low/moderate-density and gravitationally bound state (i.e. Galactic type) emerges as the most likely one. The rest remain compatible with a warm and gravitationally unbound low-density phase often found in ULIRGs. Such degeneracies, prominent when only the low-J SLED segment (J = 10, 21 and 32) is available, advise against using its CO line ratios and the so-called X(co) = M(H(2))/L(co)(10) factor as SF mode indicators, a practice that may have led to the misclassification of the ISM environments of IR-selected gas-rich discs in the distant Universe. Finally, we expect that the wide range of ISM conditions found among LIRGs will strongly impact the X(co) factor, an issue we examine in detail in Paper II.

Record 75 of 193

The Stellar and Gas Kinematics of the Little Things Dwarf Irregular Galaxy NGC 1569

Johnson, Megan; Hunter, Deidre A.; Oh, Se-Heon; Zhang, Hong-Xin; Elmegreen, Bruce; Brinks, Elias; Tollerud, Erik; Herrmann, Kimberly


卷: 144; 期: 4; 页: 152-173

In order to understand the formation and evolution of Magellanic-type dwarf irregular (dIm) galaxies, one needs to understand their three-dimensional structure. We present measurements of the stellar velocity dispersion in NGC 1569, a nearby post-starburst dIm

galaxy. The stellar vertical velocity dispersion, sigma(z), coupled with the maximum rotational velocity derived from H I observations, V-max, gives a measure of how kinematically hot the galaxy is, and, therefore, indicates its structure. We conclude that the stars in NGC 1569 are in a thick disk with a V-max/sigma(z) = 2.4 +/- 0.7. In addition to the structure, we analyze the ionized gas kinematics from O III observations along the morphological major axis. These data show evidence for outflow from the inner starburst region and a potential expanding shell near supermassive star cluster (SSC) A. When compared to the stellar kinematics, the velocity dispersion of the stars increases in the region of SSC A supporting the hypothesis of an expanding shell. The stellar kinematics closely follow the motion of the gas. Analysis of high-resolution H I data clearly reveals the presence of an H I cloud that appears to be impacting the eastern edge of NGC 1569. Also, an ultra-dense H I cloud can be seen extending to the west of the impacting H I cloud. This dense cloud is likely the remains of a dense H I bridge that extended through what is now the central starburst area. The impacting Hi cloud was the catalyst for the starburst, thus turning the dense gas into stars over a short timescale, similar to 1 Gyr. We performed a careful study of the spectral energy distribution using infrared, optical, and ultraviolet photometry, producing a state-of-the-art mass model for the stellar disk. This mass modeling shows that stars dominate the gravitational potential in the inner 1 kpc. The dynamical mass of NGC 1569, derived from V-max, shows that the disk may be dark matter deficient in the inner region, although, when compared to the expected virial mass determined from halo abundance matching techniques, the dark matter profile seems to agree with the observed mass profile at a radius of 2.2 kpc.

Record 76 of 193

Major-Merger Galaxy Pairs In the Cosmos Field-Mass-Dependent Merger Rate Evolution since z=1

Xu, C. Kevin; Zhao, Yinghe; Scoville, N.; Capak, P.; Drory, N.; Gao, Y.


卷: 747; 期: 2; 页: 85-101

We present results of a statistical study of the cosmic evolution of the mass-dependent major-merger rate since z = 1. A stellar mass limited sample of close major-merger pairs (the CPAIR sample) was selected from the archive of the COSMOS survey. Pair fractions at different redshifts derived using the CPAIR sample and a local K-band-selected pair sample show no significant variations with stellar mass. The pair fraction exhibits moderately strong cosmic evolution, with the best-fitting function of f(pair) = 10(-1.88(+/- 0.03))(1 + z)(2.2(+/- 0.2)). The best-fitting function for the merger rate is R-mg (Gyr(-1)) = 0.053 x (M-star/10(10.7) M-circle dot)(0.3)(1 + z)(2.2)/(1 + z/8). This rate implies that galaxies of M-star similar to


41

10(10)-10(11.5)M(circle dot) have undergone similar to 0.5-1.5 major mergers since z = 1. Our results show that, for massive galaxies (M-star >= 10(10.5)M(circle dot)) at z <= 1, major mergers involving star-forming galaxies (i.e., wet and mixed mergers) can account for the formation of both ellipticals and red quiescent galaxies (RQGs). On the other hand, major mergers cannot be responsible for the formation of most low mass ellipticals and RQGs of M-star less than or similar to 10(10.3)M(circle dot). Our quantitative estimates indicate that major mergers have significant impact on the stellar mass assembly of the most massive galaxies (M-star >= 10(11.3)M(circle dot)), but for less massive galaxies the stellar mass assembly is dominated by the star formation. Comparison with the mass-dependent (ultra) luminous infrared galaxies ((U)LIRG) rates suggests that the frequency of major-merger events is comparable to or higher than that of (U)LIRGs.

Record 77 of 193

Stellar Populations of Classical and Pseudo-Bulges for a Sample of Isolated Spiral Galaxies

Zhao, Yinghe


卷: 337; 期: 2; 页: 719-728

In this paper we present the stellar population synthesis results for a sample of 75 bulges in isolated spiral Sb-Sc galaxies, using the spectroscopic data from the Sloan Digital Sky Survey and the STARLIGHT code. We find that both pseudo-bulges and classical bulges in our sample are predominantly composed of old stellar populations, with mean mass-weighted stellar age around 10 Gyr. While the stellar population of pseudo-bulges is, in general, younger than that of classical bulges, the difference is not significant, which indicates that it is hard to distinguish pseudo-bulges from classical bulges, at least for these isolated galaxies, only based on their stellar populations. Pseudo-bulges have star formation activities with relatively longer timescale than classical bulges, indicating that secular evolution is more important in this kind of systems. Our results also show that pseudo-bulges have a lower stellar velocity dispersion than their classical counterparts, which suggests that classical bulges are more dispersion-supported than pseudo-bulges.

Record 78 of 193

Large-Scale Kinematics, Astrochemistry, and Magnetic Field Studies of Massive Star-Forming Regions through HC3N, HNC, and C2H Mappings

Li, Juan; Wang, Junzhi; Gu, Qiusheng; Zhang, Zhi-yu; Zheng, Xingwu


卷: 745; 期: 1; 页: 47-75

We have mapped 27 massive star-forming regions associated with water masers using three dense gas tracers: HC3N 10-9, HNC 1-0, and C2H 1-0. The FWHM

sizes of HNC clumps and C2H clumps are about 1.5 and 1.6 times higher than those of HC3N, respectively, which can be explained by the fact that HC3N traces more dense gas than HNC and C2H. We found evidence for an increase in the optical depth of C2H with a "radius" from the center to the outer regions in some targets, supporting the chemical model of C2H. The C2H optical depth is found to decline as molecular clouds evolve to a later stage, suggesting that C2H might be used as a "chemical clock" for molecular clouds. The large-scale kinematic structure of clouds was investigated with three molecular lines. All of these sources show significant velocity gradients. The magnitudes of gradient are found to increase toward the inner region, indicating the differential rotation of clouds. Both the ratio of rotational to gravitational energy and the specific angular momentum seem to decrease toward the inner region, implying the obvious angular momentum transfer, which might be caused by magnetic braking. The average magnetic field strength and number density of molecular clouds is derived using the uniform magnetic sphere model. The derived magnetic field strengths range from 3 to 88 mu G, with a median value of 13 mu G. The mass-to-flux ratio of the molecular cloud is calculated to be much higher than the critical value with derived parameters, which agrees well with numerical simulations.

Record 79 of 193

The Global Star Formation Law of Galaxies Revisited In the Radio Continuum

Liu, LiJie; Gao Yu

SCIENCE CHINA-PHYSICS MECHANICS & ASTRONOMY

卷: 55; 期: 2; 页: 347-353

We study the global star formation law, the relation between the gas and star formation rate (SFR) in a sample of 130 local galaxies with infrared (IR) luminosities spanning over three orders of magnitude (10(9)-10(12) L-aS (TM)), which includes 91 normal spiral galaxies and 39 (ultra)luminous IR galaxies [(U)LIRGs]. We derive their total (atomic and molecular) gas and dense molecular gas masses using newly available HI, CO and HCN data from the literature. The SFR of galaxies is determined from total IR (8-1000 mu m) and 1.4 GHz radio continuum (RC) luminosities. The galaxy disk sizes are defined by the de-convolved elliptical Gaussian FWHM of the RC maps. We derive the galaxy disk-averaged SFRs and various gas surface densities, and investigate their relationships. We find that the galaxy disk-averaged surface density of dense molecular gas mass has the tightest correlation with that of SFR (scatter similar to 0.26 dex), and is linear in log-log space (power-law slope of N=1.03 +/- 0.02) across the full galaxy sample. The correlation between the total gas and SFR surface densities for the full sample has a somewhat larger scatter (similar to 0.48 dex), and is best fit by a power-law with slope 1.45 +/- 0.02. However, the slope changes from similar to 1 when only normal spirals are considered, to similar to


42

1.5 when more and more (U)LIRGs are included in the fitting. When different CO-to-H-2 conversion factors are used to infer molecular gas masses for normal galaxies and (U)LIRGs, the bi-modal relations claimed recently in CO observations of high-redshift galaxies appear to also exist in local populations of star-forming galaxies.

Record 80 of 193

Tidal Dwarf Galaxies at Intermediate Redshifts

Wen, Zhang-Zheng; Zheng, Xian-Zhong; Zhao, Ying-He; Gao, Yu


卷: 337; 期: 2; 页: 729-737

We present the first attempt at measuring the production rate of tidal dwarf galaxies (TDGs) and estimating their contribution to the overall dwarf population. Using HST/ACS deep imaging data from GOODS and GEMS surveys in conjunction with photometric redshifts from COMBO-17 survey, we performed a morphological analysis for a sample of merging/interacting galaxies in the Extended Chandra Deep Field South and identified tidal dwarf candidates in the rest-frame optical bands. We estimated a production rate about 1.4 x 10(-5) per Gyr per comoving volume for long-lived TDGs with stellar mass 3x10(8-9) M-circle dot at 0.5 < z < 1.1. Together with galaxy merger rates and TDG survival rate from the literature, our results suggest that only a marginal fraction (less than 10%) of dwarf galaxies in the local universe could be tidally-originated. TDGs in our sample are on average bluer than their host galaxies in the optical. Stellar population modelling of optical to near-infrared spectral energy distributions (SEDs) for two TDGs favors a burst component with age 400/200 Myr and stellar mass 40%/26% of the total, indicating that a young stellar population newly formed in TDGs. This is consistent with the episodic star formation histories found for nearby TDGs.

Record 81 of 193

Outside-In Shrinking Of the Star-Forming Disk of Dwarf Irregular Galaxies

Zhang, Hong-Xin; Hunter, Deidre A.; Elmegreen, Bruce G.; Gao, Yu; Schruba, Andreas


卷: 143; 期: 2; 页: 47-73

We have studied multi-band surface brightness profiles of a representative sample of 34 nearby dwarf irregular galaxies. Our data include Galaxy Evolution Explorer (GALEX) FUV/NUV, UBV, and Ha and Spitzer 3.6 mu m images. These galaxies constitute the majority of the LITTLE THINGS survey (Local Irregulars That Trace Luminosity Extremes The H I Nearby Galaxy Survey). By modeling the azimuthal averages of the spectral energy distributions with a complete library of star formation histories, we derived the stellar mass surface density distributions and the star formation rate averaged over

three different timescales: the recent 0.1 Gyr, 1 Gyr, and a Hubble time. We find that, for similar to 80% (27 galaxies) of our sample galaxies, radial profiles (at least in the outer part) at shorter wavelengths, corresponding to younger stellar populations, have shorter disk scale lengths than those at longer wavelengths, corresponding to older stellar populations. This indicates that the star-forming disk has been shrinking. In addition, the radial distributions of the stellar mass surface density are well described as piece-wise exponential profiles, and similar to 80% of the galaxies have steeper mass profiles in the outer disk than in the inner region. The steep radial decline of the star formation rate in the outer parts compared to that in the inner disks gives a natural explanation for the down-bending stellar mass surface density profiles. Within the inner disks, our sample galaxies on average have constant ratios of recent star formation rate to stellar mass with radius. Nevertheless, similar to 35% (12 galaxies, among which 7 have baryonic mass less than or similar to 10(8) M-circle dot) of the sample exhibit negative slopes across the observed disk, which is in contrast with the so-called inside out disk growth scenario suggested for luminous spiral galaxies. The tendency of star formation to become concentrated toward the inner disks in low-mass dwarf irregular galaxies is interpreted as a result of their susceptibility to environmental effects and regulation through stellar feedback.

Record 82 of 193

In-Spiraling Clumps in Blue Compact Dwarf Galaxies

Elmegreen, Bruce G.; Zhang, Hong-Xin; Hunter, Deidre A.


卷: 747; 期: 2; 页: 105-113

Giant star formation clumps in dwarf irregular galaxies can have masses exceeding a few percent of the galaxy mass enclosed inside their orbital radii. They can produce sufficient torques on dark matter halo particles, halo stars, and the surrounding disk to lose their angular momentum and spiral into the central region in 1 Gyr. Pairs of giant clumps with similarly large relative masses can interact and exchange angular momentum to the same degree. The result of this angular momentum loss is a growing central concentration of old stars, gas, and star formation that can produce a long-lived starburst in the inner region, identified with the blue compact dwarf (BCD) phase. This central concentration is proposed to be analogous to the bulge in a young spiral galaxy. Observations of star complexes in five local BCDs confirm the relatively large clump masses that are expected for this process. The observed clumps also seem to contain old field stars, even after background light subtraction, in which case the clumps may be long-lived. The two examples with clumps closest to the center have the largest relative clump masses and the greatest contributions from old stars. An additional indication that the dense central regions


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of BCDs are like bulges is the high ratio of the inner disk scale height to the scale length, which is comparable to 1 for four of the galaxies.

Record 83 of 193

Molecular Gas in Infrared Ultraluminous QSO Hosts

Xia, X. Y.; Gao, Y.; Hao, C. -N.; Tan, Q. H.; Mao, S.; Omont, A.; Flaquer, B. O.; Leon, S.; Cox, P.


卷: 750; 期: 2; 页: 92-104

We report CO detections in 17 out of 19 infrared ultraluminous QSO (IR QSO) hosts observed with the IRAM 30 m telescope. The cold molecular gas reservoir in these objects is in a range of (0.2-2.1) x 10(10) M-circle dot (adopting a CO-to-H-2 conversion factor alpha CO = 0.8 M-circle dot (K km s(-1) pc(2))(-1)). We find that the molecular gas properties of IR QSOs, such as the molecular gas mass, star formation efficiency (L-FIR/L'(CO)), and CO (1-0) line widths, are indistinguishable from those of local ultraluminous infrared galaxies (ULIRGs). A comparison of low-and high-redshift CO-detected QSOs reveals a tight correlation between L-FIR and L'(CO(1-0)) for all QSOs. This suggests that, similar to ULIRGs, the far-infrared emissions of all QSOs are mainly from dust heated by star formation rather than by active galactic nuclei (AGNs), confirming similar findings from mid-infrared spectroscopic observations by Spitzer. A correlation between the AGN-associated bolometric luminosities and the CO line luminosities suggests that star formation and AGNs draw from the same reservoir of gas and there is a link between star formation on similar to kpc scale and the central black hole accretion process on much smaller scales.

Record 84 of 193

The Molecular Gas in Luminous Infrared Galaxies. II. Extreme Physical Conditions and Their Effects on the X-Co Factor

Papadopoulos, Padelis P.; van der Werf, Paul; Xilouris, E.; Isaak, Kate G.; Gao, Yu


卷: 751; 期: 1; 页: 10-38

In this work, we conclude the analysis of our CO line survey of luminous infrared galaxies (LIRGs: L-IR greater than or similar to 10(11) L-circle dot) in the local universe (Paper I) by focusing on the influence of their average interstellar medium (ISM) properties on the total molecular gas mass estimates via the so-called X-co = M(H-2)/L-co,L-1-0 factor. One-phase radiative transfer models of the global CO spectral line energy distributions (SLEDs) yield an X-co distribution with < X-co > similar to (0.6 +/- 0.2) M-circle dot (K km s(-1) pc(2))(-1) over a significant range of average gas densities, temperatures, and dynamic states. The latter emerges as the most important parameter in determining X-co, with unbound states yielding low

values and self-gravitating states yielding the highest ones. Nevertheless, in many (U)LIRGs where available higher-J CO lines (J = 3-2, 4-3, and/or J = 6-5) or HCN line data from the literature allow a separate assessment of the gas mass at high densities (>= 10(4) cm(-3)) rather than a simple one-phase analysis, we find that near-Galactic X-co similar to (3-6) M-circle dot (K km s(-1) pc(2))(-1) values become possible. We further show that in the highly turbulent molecular gas in ULIRGs, a high-density component will be common and can be massive enough for its high X-co to dominate the average value for the entire galaxy. Using solely low-J CO lines to constrain X-co in such environments (as has been the practice up until now) may have thus resulted in systematic underestimates of molecular gas mass in ULIRGs, as such lines are dominated by a warm, diffuse, and unbound gas phase with low X-co but very little mass. Only well-sampled high-J CO SLEDs (J = 3-2 and higher) and/or multi-J observations of heavy rotor molecules (e.g., HCN) can circumvent such a bias, and the latter type of observations may have actually provided early evidence of it in local ULIRGs. The only way that the global X-co of such systems could be significantly lower than Galactic is if the average dynamic state of the dense gas is strongly gravitationally unbound. This is an unlikely possibility that must nevertheless be examined, with lines of rare isotopologues of high gas density tracers (e.g., (HCN)-C-13, high-J (CO)-C-13 lines) being very valuable in yielding (along with the lines of the main isotopes) such constraints. For less IR-luminous, disk-dominated systems, we find that the galaxy-averaged X-co deduced by one-phase models of global SLEDs can also underestimate the total molecular gas mass when much of it lies in an star-formation-quiescent phase extending beyond a central star-forming region. This is because such a phase (and its large X-co) remains inconspicuous in global CO SLEDs. Finally, detailed studies of a subsample of galaxies find ULIRGs with large amounts (similar to 10(9) M-circle dot) of very warm (>= 100 K) and dense gas (>= 10(5) cm(-3)), which could represent a serious challenge to photon-dominated regions as the main energy portals in the molecular ISM of such systems.

Record 85 of 193

H I Power Spectra and the Turbulent Interstellar Medium of Dwarf Irregular Galaxies

Zhang, Hong-Xin; Hunter, Deidre A.; Elmegreen, Bruce G.


卷: 754; 期: 1; 页: 29-42

H I spatial power spectra were determined for a sample of 24 nearby dwarf irregular galaxies selected from the Local Irregulars That Trace Luminosity Extremes-The H I Nearby Galaxy Survey sample. The two-dimensional power spectral indices asymptotically become a constant for each galaxy when a significant part of the line profile is integrated. For narrow channel maps, the


44

power spectra become shallower as the channel width decreases, and this shallowing trend continues to our single channel maps. This implies that even the highest velocity resolution of 1.8 kms(-1) is not smaller than the thermal dispersion of the coolest, widespread H I component. The one-dimensional power spectra of azimuthal profiles at different radii suggest that the shallower power spectra for narrower channel width is mainly contributed by the inner disks, which indicates that the inner disks have proportionally more cooler H I than the outer disks. Galaxies with lower luminosity (M-B > -14.5 mag) and star formation rate (SFR, log(SFR (M-circle dot yr(-1))) < -2.1) tend to have steeper power spectra, which implies that the H I line-of-sight depths can be comparable with the radial length scales in low-mass galaxies. A lack of a correlation between the inertial-range spectral indices and SFR surface density implies that either non-stellar power sources are playing a fundamental role in driving the interstellar medium turbulent structure or the nonlinear development of turbulent structures has little to do with the driving sources.

Record 86 of 193

A Herschel Survey of Cold Dust in Disks around Brown Dwarfs and Low-Mass Stars

Harvey, Paul M.; Henning, Thomas; Liu, Yao; Menard, Francois; Pinte, Christophe; Wolf, Sebastian; Cieza, Lucas A.; Evans, Neal J., II; Pascucci, Ilaria


卷: 755; 期: 1; 页: 67-79

We report the complete photometric results from our Herschel study which is the first comprehensive program to search for far-infrared emission from cold dust around young brown dwarfs (BDs). We surveyed 50 fields containing 51 known or suspected BDs and very low mass stars that have evidence of circumstellar disks based on Spitzer photometry and/or spectroscopy. The objects with known spectral types range from M3 to M9.5. Four of the candidates were subsequently identified as extragalactic objects. Of the remaining 47 we have successfully detected 36 at 70 mu m and 14 at 160 mu m with signal-to-noise ratio (S/N) greater than 3, as well as several additional possible detections with low S/N. The objects exhibit a range of [24]-[70] mu m colors suggesting a range in mass and/or structure of the outer disk. We present modeling of the spectral energy distributions of the sample and discuss trends visible in the data. Using two Monte Carlo radiative transfer codes we investigate disk masses and geometry. We find a very wide range in modeled total disk masses from less than 10(-6) M-circle dot up to 10(-3) M-circle dot with a median disk mass of the order of 3 x 10(-5) M-circle dot, suggesting that the median ratio of disk

mass to central object mass may be lower than for T Tauri stars. The disk scale heights and flaring angles, however, cover a range consistent with those seen around T Tauri stars. The host clouds in which the young BDs and low-mass stars are located span a range in estimated age from similar to 1-3 Myr to similar to 10 Myr and represent a variety of star-forming environments. No obvious dependence on cloud location or age is seen in the disk properties, though the statistical significance of this conclusion is not strong.

Record 87 of 193

Different Evolutionary Stages in the Massive Star-Forming Region W3 Main Complex

Wang, Yuan; Beuther, Henrik; Zhang, Qizhou; Bik, Arjan; Rodon, Javier A.; Jiang, Zhibo; Fallscheer, Cassandra


卷: 754; 期: 2; 页: 87-108

We observed three high-mass star-forming regions in the W3 high-mass star formation complex with the Submillimeter Array and IRAM 30 m telescope. These regions, i.e., W3 SMS1 (W3 IRS5), SMS2 (W3 IRS4) and SMS3, are in different evolutionary stages and are located within the same large-scale environment, which allows us to study rotation and outflows as well as chemical properties in an evolutionary sense. While we find multiple millimeter continuum sources toward all regions, these three subregions exhibit different dynamical and chemical properties, which indicate that they are in different evolutionary stages. Even within each subregion, massive cores of different ages are found, e. g., in SMS2, sub-sources from the most evolved ultracompact HII region to potential starless cores exist within 30,000 AU of each other. Outflows and rotational structures are found in SMS1 and SMS2. Evidence for interactions between the molecular cloud and the HII regions is found in the (CO)-C-13 channel maps, which may indicate triggered star formation.

Record 88 of 193

LAMOST Experiment for Galactic Understanding and Exploration (LEGUE) - The Survey's Science Plan

Deng, Li-Cai; Newberg, Heidi Jo; Liu, Chao; Carlin, Jeffrey L.; Beers, Timothy C.; Chen, Li; Chen, Yu-Qin; Christlieb, Norbert; Grillmair, Carl J.; Guhathakurta, Puragra; Han, Zhan-Wen; Hou, Jin-Liang; Lee, Hsu-Tai; Lepine, Sebastien; Li, Jing; Liu, Xiao-Wei; Pan, Kai-Ke; Sellwood, J. A.; Wang, Bo; Wang, Hong-Chi; Yang, Fan; Yanny, Brian; Zhang, Hao-Tong; Zhang, Yue-Yang; Zheng, Zheng; Zhu, Zi


卷: 12; 期: 7; 页: 735-754

We describe the current plans for a spectroscopic survey of millions of stars in the Milky Way galaxy using the Guo Shou Jing Telescope (GSJT, formerly called the Large sky Area Multi-Object fiber Spectroscopic Telescope - LAMOST). The survey will obtain spectra for

Molecular Clouds and Star Formation


45

2.5 million stars brighter than r < 19 during dark/grey time, and 5 million stars brighter than r < 17 or J < 16 on nights that are moonlit or have low transparency. The survey will begin in the fall of 2012, and will run for at least four years. The telescope's design constrains the optimal declination range for observations to 10 degrees < delta < 50 degrees, and site conditions lead to an emphasis on stars in the direction of the Galactic anticenter. The survey is divided into three parts with different target selection strategies: disk, anticenter, and spheroid. The resulting dataset will be used to study the merger history of the Milky Way, the substructure and evolution of the disks, the nature of the first generation of stars through identification of the lowest metallicity stars, and star formation through study of open clusters and OB associations. Detailed design of the LAMOST Experiment for Galactic Understanding and Exploration (LEGUE) survey will be completed in summer 2012, after a review of the results of the pilot survey.

Record 89 of 193

An Algorithm for Preferential Selection of Spectroscopic Targets in LEGUE

Carlin, Jeffrey L.; Lepine, Sebastien; Newberg, Heidi Jo; Deng, Li-Cai; Beers, Timothy C.; Chen, Yu-Qin; Christlieb, Norbert; Fu, Xiao-Ting; Gao, Shuang; Grillmair, Carl J.; Guhathakurta, Puragra; Han, Zhan-Wen; Hou, Jin-Liang; Lee, Hsu-Tai; Li, Jing; Liu, Chao; Liu, Xiao-Wei; Pan, Kai-Ke; Sellwood, J. A.; Wang, Hong-Chi; Yang, Fan; Yanny, Brian; Zhang, Yue-Yang; Zheng, Zheng; Zhu, Zi


卷: 12; 期: 7; 页: 755-771

We describe a general target selection algorithm that is applicable to any survey in which the number of available candidates is much larger than the number of objects to be observed. This routine aims to achieve a balance between a smoothly-varying, well-understood selection function and the desire to preferentially select certain types of targets. Some target-selection examples are shown that illustrate different possibilities of emphasis functions. Although it is generally applicable, the algorithm was developed specifically for the LAMOST Experiment for Galactic Understanding and Exploration (LEGUE) survey that will be carried out using the Chinese Guo Shou Jing Telescope. In particular, this algorithm was designed for the portion of LEGUE targeting the Galactic halo, in which we attempt to balance a variety of science goals that require stars at fainter magnitudes than can be completely sampled by LAMOST. This algorithm has been implemented for the halo portion of the LAMOST pilot survey, which began in October 2011.

Record 90 of 193

The Site Conditions of the Guo Shou Jing Telescope

Yao, Song; Liu, Chao; Zhang, Hao-Tong; Deng, Li-Cai; Newberg, Heidi Jo; Zhang, Yue-Yang; Li, Jing; Liu, Nian;

Zhou, Xu; Carlin, Jeffrey L.; Chen, Li; Christlieb, Norbert; Gao, Shuang; Han, Zhan-Wen; Hou, Jin-Liang; Lee, Hsu-Tai; Liu, Xiao-Wei; Pan, Kai-Ke; Wang, Hong-Chi; Xu, Yan; Yang, Fan


卷: 12; 期: 7; 页: 772-780

The weather at the Xing long Observing Station, where the Guo Shou Jing Telescope (GSJT) is located, is strongly affected by the monsoon climate in north-east China. The LAMOST survey strategy is constrained by these weather patterns. We present statistics on observing hours from 2004 to 2007, and the sky brightness, seeing, and sky transparency from 1995 to 2011 at the site. We investigate effects of the site conditions on the survey plan. Operable hours each month show a strong correlation with season: on average there are eight operable hours per night available in December, but only one two hours in July and August. The seeing and the sky transparency also vary with season. Although the seeing is worse in windy winters, and the atmospheric extinction is worse in the spring and summer, the site is adequate for the proposed scientific program of the LAMOST survey. With a Monte Carlo simulation using historical data on the site condition, we find that the available observation hours constrain the survey footprint from 22(h) to 16(h) in right ascension; the sky brightness allows LAMOST to obtain a limiting magnitude of V = 19.5 mag with S/N= 10.

Record 91 of 193

The LEGUE Input Catalog for Dark Night Observing in the LAMOST Pilot Survey

Yang, Fan; Carlin, Jeffrey L.; Liu, Chao; Zhang, Yue-Yang; Gao, Shuang; Xu, Yan; Deng, Li-Cai; Newberg, Heidi Jo; Lepine, Sebastien; Hou, Jin-Liang; Liu, Xiao-Wei; Christlieb, Norbert; Zhang, Hao-Tong; Lee, Hsu-Tai; Pan, Kai-Ke; Han, Zhan-Wen; Wang, Hong-Chi


卷: 12; 期: 7; 页: 781-791

We outline the design of the dark nights portion of the LAMOST Pilot Survey, which began observations in 2011 October. In particular, we focus on Milky Way stellar candidates that are targeted for the LEGUE (LAMOST Experiment for Galactic Understanding and Exploration) survey. We discuss the regions of sky in which spectroscopic candidates were selected, and the motivations for selecting each of these sky areas. Some limitations due to the unique design of the telescope are discussed, including the requirement that a bright (V < 8) star be placed at the center of each plate for wavefront sensing and active optics corrections. The target selection categories and scientific goals motivating them are briefly discussed, followed by a detailed overview of how these selection functions were implemented. We illustrate the difference between the overall input catalog - Sloan Digital Sky Survey (SDSS) photometry and the final targets selected


46

for LAMOST observations.

Record 92 of 193

The LEGUE High Latitude Bright Survey Design For the LAMOST Pilot Survey

Zhang, Yue-Yang; Carlin, Jeffrey L.; Yang, Fan; Liu, Chao; Deng, Li-Cai; Newberg, Heidi Jo; Zhang, Hao-Tong; Lepine, Sebastien; Xu, Yan; Gao, Shuang; Christlieb, Norbert; Han, Zhan-Wen; Hou, Jin-Liang; Lee, Hsu-Tai; Liu, Xiao-Wei; Pan, Kai-Ke; Wang, Hong-Chi


卷: 12; 期: 7; 页: 792-804

We describe the footprint and input catalog for bright nights in the LAMOST Pilot Survey, which began in October 2011. Targets are selected from two stripes in the north and south Galactic Cap regions, centered at delta = 29 degrees, with 10 degrees width in declination, covering right ascensions of 135 degrees to 290 degrees and -30 degrees to 30 degrees respectively. We selected spectroscopic targets from a combination of the SDSS and 2MASS point source catalogs. The catalog of stars defining the field centers (as required by the Shack-Hartmann wavefront sensor at the center of the LAMOST field) consists of all V < 8(m) stars from the Hipparcos catalog. We employ a statistical selection algorithm that assigns priorities to targets based on their positions in multidimensional color/magnitude space. This scheme overemphasizes rare objects and de-emphasizes more populated regions of magnitude and color phase space, while ensuring a smooth, well-understood selection function. A demonstration of plate design is presented based on the Shack-Hartmann star catalog and an input catalog that was generated by our target selection routines.

Record 93 of 193

The LEGUE Disk Targets for LAMOST's Pilot Survey

Chen, Li; Hou, Jin-Liang; Yu, Jin-Cheng; Liu, Chao; Deng, Li-Cai; Newberg, Heidi Jo; Carlin, Jeffrey L.; Yang, Fan; Zhang, Yue-Yang; Shen, Shi-Yin; Zhang, Hao-Tong; Chen, Jian-Jun; Chen, Yu-Qin; Christlieb, Norbert; Han, Zhan-Wen; Lee, Hsu-Tai; Liu, Xiao-Wei; Pan, Kai-Ke; Shi, Jian-Rong; Wang, Hong-Chi; Zhu, Zi


卷: 12; 期: 7; 页: 805-812

We describe the target selection algorithm for the low latitude disk portion of the LAMOST Pilot Survey, which aims to test systems in preparation for the LAMOST spectroscopic survey. We use the PPMXL astrometric catalog, which provides positions, proper motions, B/R/I magnitudes (mostly) from USNO-B and J/H/Ks from the Two Micron All Sky Survey (2MASS) as well. We chose eight plates along the Galactic plane, in the region 0 degrees < alpha < 67 degrees and 42 degrees < delta < 59 degrees, which cover 22 known open clusters with a range of ages. Adjacent plates may have some small overlapping area. Each plate covers an area of 2.5

degrees in radius, with its central star (for the Shack-Hartmann guider) brighter than 8th magnitude. For each plate, we create an input catalog in the magnitude range 11.3 < I-mag < 16.3 and B-mag available from PPMXL. The stars are selected to satisfy the requirements of the fiber positioning system and have a uniform distribution in the I vs. B - I color-magnitude diagram. Our final input catalog consists of 12 000 objects on each of eight plates that are observable during the winter observing season from the Xing long Station of the National Astronomical Observatory of China.

Record 94 of 193

A Resonant Feature near The Perseus Arm Revealed by Red Clump Stars

Liu, Chao; Xue, Xiangxiang; Fang, Min; van de Ven, Glenn; Wu, Yue; Smith, Martin C.; Carrell, Kenneth


卷: 753; 期: 1; 页: L24-L26

We investigate the extinction, together with the radial velocity (RV) dispersion and distribution of red clump stars in the anticenter direction using spectra obtained with Hectospec on the MMT. We find that extinction peaks at Galactocentric radii of about 9.5 and 12.5 kpc, right in front of the locations of the Perseus and Outer arms and in line with the relative position of dust and stars in external spiral galaxies. The RV dispersion peaks around 10 kpc, which coincides with the location of the Perseus arm, yields an estimated arm-interarm density contrast of 1.3-1.5, and is in agreement with previous studies. Finally, we discover that the RV distribution bifurcates around 10-11 kpc into two peaks at +27 km s(-1) and -4 km s(-1). This seems to be naturally explained by the presence of the outer Lindblad resonance of the Galactic bar, but further observations will be needed to understand if the corotation resonance of the spirals arms also plays a role.

Record 95 of 193

A Population of Isolated Hard X-Ray Sources near The Supernova Remnant Kes 69

Bocchino, F.; Bykov, A. M.; Chen, Y.; Krassilchtchikov, A. M.; Levenfish, K. P.; Miceli, M.; Pavlov, G. G.; Uvarov, Yu. A.; Zhou, X.


卷: 541; 页: A152-1-A152-9

Recent X-ray observations of the supernova remnant (SNR) IC 443 interacting with molecular clouds detected a new population of hard X-ray sources related to the remnant itself, which has been proposed to be fast ejecta fragments propagating within the dense environment. Encouraged by these studies, we obtained a deep XMM-Newton observation of the SNR Kes 69, which also shows signs of a shock-cloud interaction. We report on the detection of 18 hard X-ray sources in the field of Kes 69, which is a number


47

sognificantly higher than expected for the Galactic source population in the field. The sources are spatially correlated with CO emission from the cloud in the remnant environment. The spectra of 3 of the 18 sources can be described as hard power-laws with photon indices smaller than two plus line emission associated with K-shell transitions. We discuss the two most promising scenarios for the interpretation of the sources, namely fast ejecta fragments (as in IC 443) and cataclysmic variables. While most of the observational evidence is consistent with the former interpretation, we cannot rule out the latter.

Record 96 of 193

Star formation and disk properties in Pismis 24

Fang, M.; van Boekel, R.; King, R. R.; Henning, Th.; Bouwman, J.; Doi, Y.; Okamoto, Y. K.; Roccatagliata, V.; Sicilia-Aguilar, A.


卷: 539; 页: A119-1-A119-21

Context. Circumstellar disks are expected to evolve quickly in massive young clusters harboring many OB-type stars. Two processes have been proposed to drive the disk evolution in such cruel environments: (1) gravitational interaction between circumstellar disks and nearby passing stars (stellar encounters); and (2) photoevaporation by UV photons from massive stars. The relative importance of both mechanisms is not well understood. Studies of massive young star clusters can provide observational constraints on the processes of driving disk evolution.Aims. We investigate the properties of young stars and their disks in the NGC 6357 complex, concentrating on the most massive star cluster within the complex: Pismis 24.Methods. We use infrared data from the 2MASS and Spitzer GLIMPSE surveys, complemented with our own deep Spitzer imaging of the central regions of Pismis 24, in combination with X-ray data to search for young stellar objects (YSOs) in NGC 6357 complex. The infrared data constrain the disk presence and are complemented by optical photometric and spectroscopic observations, obtained with VLT/VIMOS, that constrain the properties of the central stars. For those stars with reliable spectral types we combine spectra and photometry to estimate the mass and age. For cluster members without reliable spectral types we obtain the mass and age probability distributions from R and I-band photometry, assuming these stars have the same extinction distribution as those in the "spectroscopic" sample. We compare the disk properties in the Pismis 24 cluster with those in other clusters/star-forming regions employing infrared color-color diagrams.Results. We discover two new young clusters in the NGC 6357 complex. We give a revised distance estimate for Pismis 24 of 1.7 +/- 0.2 kpc. We find that the massive star Pis 24-18 is a binary system, with the secondary being the main X-ray source of the pair. We provide photometry in 9 bands between 0.55 and 9 mu m for the members of the Pismis 24 cluster. We derive the cluster mass

function and find that up to the completeness limit at low masses it agrees well with the initial mass function of the Trapezium cluster. We derive a median age of 1 Myr for the Pismis 24 cluster members. We find five proplyds in HST archival imaging of the cluster, four of which are newly found. In all cases the proplyd tails are pointing directly away from the massive star system Pis 24-1. One proplyd shows a second tail, pointing away from Pis 24-2, suggesting this object is being photoevaporated from two directions simultaneously. We find that the global disk frequency (similar to 30%) in Pismis 24 is much lower than some other clusters of similar age, such as the Orion Nebula Cluster. When comparing the disk frequencies in 19 clusters/star-forming regions of various ages and different (massive) star content, we find that the disks in clusters harboring extremely massive stars (typically earlier than O5), like Pismis 24, are dissipated roughly twice as quickly as in clusters/star-forming regions without extremely massive stars. Within Pismis 24, we find that the disk frequency within a projected distance of 0.6 pc from Pis 24-1 is substantially lower than at larger radii (similar to 19% vs. similar to 37%). We argue for a combination of photoevaporation and irradiation with ionizing UV photons from nearby massive stars, causing increased MRI-induced turbulence and associated accretion activity, to play an important role in the dissipation of low-mass star disks in Pismis 24.

Record 97 of 193

Unveiling the Physical Properties and Kinematics of Molecular Gas in the Antennae Galaxies (NGC 4038/9) Through High-Resolution CO (J=3-2) Observations

Ueda, Junko; Iono, Daisuke; Petitpas, Glen; Yun, Min S.; Ho, Paul T. P.; Kawabe, Ryohei; Mao, Rui-Qing; Martin, Sergio; Matsushita, Satoki; Peck, Alison B.; Tamura, Yoichi; Wang, Junzhi; Wang, Zhong; Wilson, Christine D.; Zhang, Qizhou


卷: 745; 期: 1; 页: 65-78

We present a similar to 1 '' (100 pc) resolution (CO)-C-12 (3-2) map of the nearby intermediate-stage interacting galaxy pair NGC 4038/9 (the Antennae galaxies) obtained with the Submillimeter Array. We find that half the CO (3-2) emission originates in the overlap region where most of the tidally induced star formation had been previously found in shorter wavelength images, with the rest being centered on each of the nuclei. The gross distribution is consistent with lower resolution single-dish images, but we show for the first time the detailed distribution of the warm and dense molecular gas across this galaxy pair at resolutions comparable to the size of a typical giant molecular complex. While we find that 58% (33/57) of the spatially resolved Giant Molecular Associations (a few x 100 pc) are located in the overlap region, only <= 30% spatially coincides with the optically detected star clusters, suggesting that the bulk of the CO (3-2) emission traces the regions with very recent or near


48

future star formation activity. The spatial distribution of the CO (3-2)/CO (1-0) integrated brightness temperature ratios mainly ranges between 0.3 and 0.6, which suggests that on average the CO (3-2) line in the Antennae is not completely thermalized and similar to the average values of nearby spirals. A higher ratio is seen in both nuclei and the southern complexes in the overlap region. A higher radiation field associated with intense star formation can account for the nucleus of NGC 4038 and the overlap region, but the nuclear region of NGC 4039 shows relatively little star formation or active galactic nucleus activity and cannot be easily explained. We show kinematical evidence that the high line ratio in NGC 4039 is possibly caused by gas inflow into the counter-rotating central disk.

Record 98 of 193

Age Spread in W3 Main: Large Binocular Telescope/LUCI Near-Infrared Spectroscopy of the Massive Stellar Content

Bik, A.; Henning, Th.; Stolte, A.; Brandner, W.; Gouliermis, D. A.; Gennaro, M.; Pasquali, A.; Rochau, B.; Beuther, H.; Ageorges, N.; Seifert, W.; Wang, Y.; Kudryavtseva, N.


卷: 744; 期: 2; 页: 87-99

We present near-infrared multi-object spectroscopy and JHK(s) imaging of the massive stellar content of the Galactic star-forming region W3 Main, obtained with LUCI at the Large Binocular Telescope. We confirm 15 OB stars in W3 Main and derive spectral types between O5V and B4V from their absorption line spectra. Three massive young stellar objects are identified by their emission line spectra and near-infrared excess. The color-color diagram of the detected sources allows a detailed investigation of the slope of the near-infrared extinction law toward W3 Main. Analysis of the Hertzsprung-Russell diagram suggests that the Nishiyama extinction law fits the stellar population of W3 Main best (E(J -H)/ E(H - K-s) = 1.76 and RKs = 1.44). From our spectrophotometric analysis of the massive stars and the nature of their surrounding H II regions, we derive the evolutionary sequence of W3 Main and we find evidence of an age spread of at least 2-3 Myr. While the most massive star (IRS2) is already evolved, indications for high-mass pre-main-sequence evolution are found for another star (IRS N1), deeply embedded in an ultracompact H II (UCH II) region, in line with the different evolutionary phases observed in the corresponding H II regions. We derive a stellar mass of W3 Main of (4 +/- 1) x 10(3) M-circle dot by extrapolating from the number of OB stars using a Kroupa initial mass function and correcting for our spectroscopic incompleteness. We have detected the photospheres of OB stars from the more evolved diffuse H II region to the much younger UCH II regions, suggesting that these stars have finished their formation and cleared away their circumstellar disks very fast. Only in the hyper-compact H II region (IRS5)

do the early-type stars seem to be still surrounded by circumstellar material.

Record 99 of 193

DoAr 33: A Good Candidate for Revealing Dust Growth and Settling In Protoplanetary Disks

Y. Liu; D. Madlener; Wolf; H. Wang; J. Philipp Ruge


卷: 546; 页: A7-1-A7-8

Aims: We aim to evaluate the evolutionary stage of the circumstellar disk around DoAr 33, a T Tauri star in the Ophiuchus molecular cloud and a promising target for follow-up observations to find signs of dust evolution in protoplanetary disks. Methods: The currently available data on DoAr 33 comprises its spectral energy distribution from the optical to the millimeter regimes. This data set allows us to characterize the structure of a circumstellar disk using self-consistent radiative transfer models. We employed two different types of models, a well-mixed model and a settled disk model in which dust growth and settling are taken into account. Simulated annealing was used to search for an optimum parameter set. Results: Our results suggest that the assumption of a well-mixed dust and gas phase leads to overestimation of the mid-infrared flux, whereas the (sub)millimeter emission can be predicted quite well. Observational and theoretical arguments imply that an overall decrease in mid-infrared flux can be explained by dust growth and settling towards the midplane of the disk. As expected, the settled disk model is able to satisfactorily reproduce the data points at all wavelengths. DoAr 33 is therefore a good candidate for studying dust growth and settling in protoplanetary disks, so it deserves to be investigated with future observations.

Record 100 of 193

Type IIn SUPERNOVA SN 2010jl: Optical Observations for Over 500 Days after Explosion

Zhang, Tianmeng; Wang, Xiaofeng; Wu, Chao; Chen, Juncheng; Chen, Jia; Liu, Qin; Huang, Fang; Liang, Jide; Zhao, Xulin; Lin, Lin; Wang, Min; Dennefeld, Michel; Zhang, Jujia; Zhai, Meng; Wu, Hong; Fan, Zhou; Zou, Hu; Zhou, Xu; Ma, Jun


卷: 144; 期: 5; 页: 131-143

We present extensive optical observations of a Type IIn supernova (SN IIn) 2010jl for the first 1.5 years after its discovery. The UBVRI light curves demonstrated an interesting two-stage evolution during the nebular phase, which almost flatten out after about 90 days from the optical maximum. SN 2010jl has one of the highest intrinsic Ha luminosities ever recorded for an SN IIn, especially at late phase, suggesting a strong interaction of SN ejecta with the dense circumstellar material (CSM) ejected by the progenitor. This is also indicated by the remarkably strong Balmer lines


49

persisting in the optical spectra. One interesting spectral evolution about SN 2010jl is the appearance of asymmetry of the Balmer lines. These lines can be well decomposed into a narrow component and an intermediate-width component. The intermediate-width component showed a steady increase in both strength and blueshift with time until t similar to 400 days after maximum, but it became less blueshifted at t similar to 500 days, when the line profile appeared relatively symmetric again. Owing to the fact that a pure reddening effect will lead to a sudden decline of the light curves and a progressive blueshift of the spectral lines, we therefore propose that the asymmetric profiles of H lines seen in SN 2010jl are unlikely due to the extinction by newly formed dust inside the ejecta, contrary to the explanation by some early studies. Based on a simple CSM-interaction model, we speculate that the progenitor of SN 2010jl may suffer a gigantic mass loss (similar to 30-50 M-circle dot) a few decades before explosion. Considering a slow-moving stellar wind (e. g., similar to 28 km s(-1)) inferred for the preexisting, dense CSM shell and the extremely high mass-loss rate (1-2 M-circle dot yr(-1)), we suggest that the progenitor of SN 2010jl might have experienced a red supergiant stage and may explode finally as a post-red supergiant star with an initial mass above 30-40 M-circle dot.

Record 101 of 193

Constraints on the Dark Matter Annihilation Scenario of Fermi 130 GeV Gamma-Ray Line Emission by Continuous Gamma-Rays, Milky Way Halo, Galaxy Clusters and Dwarf

Xiaoyuan Huang; Yuan, Qiang; Peng-Fei Yin; Xiao-Jun Bi ;Xuelei Chen

Journal of Cosmology and Astroparticle Physics

卷: 2012; 期: 11; 页: 048

It was recently reported that there may exist monochromatic $\gamma$-ray emission at $\sim 130$ GeV from the Galactic center in the Fermi Large Area Telescope data, which might be related with dark matter (DM) annihilation. In this work we carry out a comprehensive check of consistency of the results with the DM annihilation scenario, using the 3.7 yrs Fermi observation of the inner Galaxy, Galactic halo, clusters of galaxies and dwarf galaxies. The results found are as follows. 1) Very strong constraints on the DM annihilation into continuous $\gamma$-rays from the Galactic center are set, which are as stringent as the "natural" scale assuming thermal freeze-out of DM. Such limit sets strong constraint on the DM models to explain the line emission. 2) No line emission from the Galactic halo is found in the Fermi data, and the constraints on line emission is marginally consistent with the DM annihilation interpretation of the $\sim 130$ GeV line emission from the inner Galaxy. 3) No line emission from galaxy clusters and dwarf galaxies is detected, although possible concentration of photons from clusters in 120-140 GeV is revealed. The

constraints from clusters and dwarf galaxies are weak and consistent with the DM annihilation scenario to explain the $\sim 130$ GeV line emission.

Record 102 of 193

Near-Infrared Imaging Polarization Study of M 17

Chen, Zhiwei; Jiang, Zhibo; Wang, Yuan; Chini, Rolf; Tamura, Motohide; Nagayama, Takahiro; Nagata, Tetsuya; Nakajima, Yasushi

Publications of the Astronomical Society of Japan

卷: 64; 期: 5; 页: 110-121

We conducted wide-field (˜8'× 8') JHKs imagingpolarimetric observations toward the massive star-formation region M 17. The southern H II bar is identified as large-scale infrared reflection nebula (IRN) illuminated by OB stars in the cluster center, while the northern bar shows polarization originating from dichroic extinction. Three small-scale bipolar IRN with centro-symmetric polarizationpatterns were identified, and their illuminating sources, embedded young stellar objects (YSOs), are most likely the driving sources of bipolar outflows. JHKs polarizations of point sources in M 17 show a wavelength dependence of the polarization of dichroic extinction in the general interstellar medium, indicating α ˜ 1.8 for the empirical

relation P ∝ λ-α

of interstellarpolarization. The

distribution of the polarization angle shows two peaks at 170° and 110°, indicating a non-uniform magnetic field structure in M 17. The direction of the magnetic field in the cluster region is south-north. However, the magnetic field in the H II region is roughly between 100°-140°, roughly perpendicular to the Galactic disk. Such a configuration indicates that the magnetic field in the cluster region is twisted from the primordial orientation in the cluster formation. The magnetic field in the southern bar has a total strength of ˜ 230μ G, and is 40° inclined to the plane of the sky. The outflows driven by YSOs in M 17 show a poor relation with the surrounding magnetic fields. This fact implies that the magnetic field in M 17 does not dominate the orientations of protostars formed inside

Record 103 of 193

Spectral Response and Noise Temperature of a 2.5 THz Spiral Antenna Coupled NbN HEB Mixer

Zhang, W; W Miao; Q j Yao; Z H LIN; S C Shi; JR Gao; G N Goltsman

Physics Procedia

卷: 36 页: 334-337

Laboratory for Millimeter &

Sub-Millimeter Wave


50

We report on a 2.5 THz spiral antenna coupled NbN hot electron bolometer (HEB) mixers, fabricated with in-situ process. The receiver noise temperature with lowest value of 1180 K is in good agreement with calculated quantum efficiency factor as a function of bias voltage. In addition, the measured spectral response of the spiral antenna coupled NbN HEB mixer shows broad frequency coverage of 0.8-3 THz, and corrected response for optical losses, FTS, and coupling efficiency between antenna and bolometer falls with frequency due to diffraction-limited beam of lens/antenna combination.

Record 104 of 193

Study on the Optics of the 5 Meter Dome A Terahertz Explorer (DATE 5) for Antarctica

Lou, Zheng; Zuo, yingxi; Cheng, Jingquan; Yang, ji; Shi, Shengcai

Antennas, Propagation & EM Theory (ISAPE), 2012 10th International Symposium on

页: 47-50

The 5 m Dome A Terahertz Explorer (DATE5) is a proposed terahertz telescope to be deployed in Dome A, Antarctica, to exploit one of the best observing conditions at terahertz bands on the earth. This paper presents a study on the optics of the proposed DATE5 antenna. Two configurations, namely the Cassegrain and the Coudé configurations, are proposed and their respective optical performances, such as field of view, beam and aperture efficiency, and chopping performance, are simulated and compared. Some engineering considerations, such as system reliability and environmental adaptability are also discussed.

Record 105 of 193

Temperature-Dependent Performances of Nb SIS Mixers at Millimeter and Submillimeter Wavelength

Liu, Jie; Wenlei Shan; Shengcai Shi

Microwave and Millimeter Wave Technology

卷: 5; 页: 1-4

The dependence of the performance of Superconductor-Insulator-Superconductor (SIS) mixers on the ambient temperature is investigated both theoretically and experimentally at millimeter and submillimeter wavelength. We found that the mixers' conversion gain plays a dominant role in the temperature-induced variation of the overall receiver sensitivity. To achieve a straightforward image of how the ambient temperature influences the conversion gain, we introduce a pure shape factor that allows for determining the mixers' conversion gain from the nonlinearity of their IV curves. We measured the performance of an SIS mixer at 100GHz band with the ambient temperature ranging from 3.8K to 8.5K to verify the validity of the quantum mixing theory. The experimental results are found in good agreement with the simulation results. This agreement indicates the

validity of quantum mixing theory at a relatively high temperature up to the superconducting critical temperature. The measurement results show that at 100GHz band, the Nb SIS mixer can maintain a reasonable performance at the ambient temperature as high as 80% of the superconducting critical temperature. In addition to the gain and noise, the receiver stability in terms of Allen variance was also measured at various ambient temperatures without any apparent difference found.

Record 106 of 193

Effects of Multiple Reflections and Low-Frequency Interferences on Measured Terahertz Fourier Transform Spectra

Li, Shao-Liang; Kang-Min Zhou; Wen-Ying Duan; Zhen-Hui Lin; Qi-Jun Yao; Sheng-Cai Shi

Proceedings of SPIE--Infrared, Millimeter-Wave, and Terahertz Technologies

卷: 8562; 页: 856204-1-856204-6

Fourier transform spectroscopy (FTS) is a measurement technique widely used in characterizing the spectrum of light sources and the frequency response of detectors. Some “ghost” spectral lines, however, are often observed in measured Fourier transform spectra, such as high-frequency harmonics of the light source due to multiple reflections in the measurement system and unexpected high frequency lines owing to low-frequency interferences in the data acquisition. Here we study the effects of multiple reflections and low-frequency interferences on the THz spectra measured by a Fourier transform spectrometer for different THz sources and detectors. Experimental and simulation results will be presented.

Record 107 of 193

A Novel Quasi-Optical Subharmonically Pumped GaAs Diode Mixer at 375 GHz

Hu, Jie; Zheng Lou; Sheng-Cai Shi


卷: 8562; 页: 85620Z-1-85620Z-6

This paper presents the design and characterization of a novel quasioptical subharmonically pumped GaAs Schottky diode mixer at 375 GHz. It features the use of two off-axis twin-slot antennas fed by CPW to receive the RF and LO signals respectively. The mixer circuits together with the antennas are integrated on a silicon extended elliptical lens. Conventional harmonic balance simulations in combination with 3D fullwave simulations in HFSS are carried out to analyze the performance of the mixer. Optimal conversion loss is obtained after impedances of the LO and RF ports are matched.Final simulation results show that the mixer achieves a DSB conversion loss of 10 dB and a noise


51

temperature of 2900 K.

Record 108 of 193

Readout System for the Terahertz Superconducting Imaging Array (TeSIA)

Li, Sheng; Jin-Ping Yang; Wen-Ying Duan; Zhen-Hui Lin; Jing Li; Sheng-Cai Shi


卷: 8562; 页: 85620L-1-85620L-5

Terahertz Superconducting Imaging Array (TeSIA) is a project for the development of a large THz direct-detection array for mapping observations. The prototype of TeSIA is an 8×8 pixel direct-detection array operating at the 850 μm band, incorporating THz superconducting detectors such as kinetic inductance detectors (KIDs) and transition edge sensors (TES). KIDs have the advantage that only a broadband low noise cryogenic amplifier is needed at low temperature for the readout system, and hundreds of pixels could be readout simultaneously by the frequency-division multiplexing (FDM) technique. The readout system for a KIDs array is composed of several parts like excitation signal generating, intermediate frequency (IF) circuit, baseband signal acquisition and processing. Excitation signal is a kind of comb signal carrying various frequencies corresponding simply to resonant frequencies of the detectors. It is generated in baseband with a bandwidth covering all KIDs and up-converted to microwave frequency (about several gigahertz) to feed the detectors. With THz radiation, the forward transmission coefficient (S21) of all KIDs varies and the variation can be measured through the comb signal. Fast Fourier transform (FFT) with pipeline structure will be used to process the baseband excitation signal in real time. Consequently, the radiation intensity can be estimated by monitoring the signal amplitude and phase of the corresponding frequency channels. In this paper we will present mainly the design ofan electronic readout system for the 8×8 pixel array.

Record 109 of 193

Atmospheric Profiling Synthetic Observation System at THz

Yao, Qijun; Dong Liu; Jing Li; Zhenhui Lin; Zheng Lou; Shengcai Shi; Hiroyuki Maezawa; Scott Paine


卷: 8562; 页: 85620T-1-85620T-9

In this paper, we will introduce a dual-THz-band SIS (Superconductor-Insulator-Superconductor) heterodyne radiometer system developed for the atmospheric profiling synthetic observation system project (APSOS). This THz system is intended to have a durable and

compact design to meet the challenging requirements of remote operation. The system as well as its major components such as antenna tipping, quasi-optics, cryogenics, SIS mixers and FFTS backend will be discussed thoroughly. Some scientific simulation focusing on the atmospheric profiling components at THz bands will also be investigated.

Record 110 of 193

Development of Superconducting Spectroscopic Array Receiver: A Multibeam 2SB SIS Receiver for Millimeter-Wave Radio Astronomy

Shan, Wenlei; Ji Yang; Shengcai Shi; Qijun Yao; Yingxi Zuo; Zhenhui Lin; Shanhuai Chen; Xuguo Zhang; Wenying Duan; Aiqing Cao; Sheng Li; Zhenqiang Li; Jie Liu; Jiaqiang Zhong

IEEE Transactions on Terahertz Science and Technology

卷: 2; 期: 6; 页: 593-604

We have developed a 3×3 multibeam sideband separation superconducting receiver-Superconducting Spectroscopic Array Receiver (SSAR)-for the 85-115 GHz frequency band. The receiver employs 2SB superconductor-insulator-superconductor (SIS) mixers with a typical single sideband (SSB) noise temperature of 60 K and image rejection ratio above 10 dB over the frequency band. Digital techniques are extensively applied in this receiver system for excellent operational stability and efficiency. They include fast Fourier spectrometers, digital LO and digital bias supplies. In our knowledge this is the first 2SB multibeam millimeter wavelength receiver in the world. This receiver has been successfully put into observation and its considerable enhancement of mapping speed has been demonstrated.

Record 111 of 193

Influence of Substrate on Coupling of High Temperature Superconducting Josephson junction Arrays

Wang, P.; Wang, Zh.; B. Fan; W. Xie; W. Liu; XJ. Zhao; X. Zhang; L. Ji; M. He; L. Fang; S.L. Yan

Physica C: Superconductivity

卷: 483; 期: 14; 页: 97-100

High temperature superconducting (HTS) Josephson junction arrays (JJAs) fabricated on bicrystal substrate were embedded in a Fabry–Pérot (F–P) resonator. We detected the radiation from the JJAs at about 74.08 GHz. By investigating the Current–Voltage (I–V) characteristics of the JJAs, the influence of the substrate on height of the Shapiro steps was studied. The result showed that the JJAs located at different positions of the substrate had different coupling strength. Also, the influence of the substrate was explored by presenting the comparison of radiation at different frequencies. Electromagnetic simulation was used to explain the


52

experiment results.

Record 112 of 193

Development of Superconducting Mixers for THz Astronomy

Shi, ShengCai

SCIENCE CHINA-INFORMATION SCIENCES

卷: 55; 期: 1; 页: 120-126

The terahertz (THz) regime, loosely defined as 0.1-10 THz, is the last frequency window to be fully explored in astronomy. In particular, it is a regime in which there are rich molecular rotation lines and atomic fine structure lines. They are very important tracers for studying the dynamics of astronomical objects such as stars and planetary systems. Observing those spectral lines usually makes use of coherent detectors (i.e., heterodyne mixers). With sensitivity approaching the quantum limit, superconducting mixers have become the coherent detector of choice in THz astronomy. In this paper we mainly introduce the superconducting mixers developed at Purple Mountain Observatory and those for international collaborative projects.

Record 113 of 193

Stabilized Hot Electron Bolometer Heterodyne Receiver at 2.5 THz

Hayton, D. J.; Gao, J. R.; Kooi, J. W.; Ren, Y.; Zhang, W.; de lange, G.

APPLIED PHYSICS LETTERS

卷: 100; 期: 8; 页: 081102-1-081102-4

We report on a method to stabilize a hot electron bolometer (HEB) mixer at 2.5 THz. The technique utilizes feedback control of the local oscillator (LO) laser power by means of a swing-arm actuator placed in the optical beam path. We demonstrate that this technique yields a factor of 50 improvement in the spectroscopic Allan variance time which is shown to be over 30 s in a 12 MHz noise fluctuation bandwidth. Furthermore, broadband signal direct detection effects may be minimized by this technique. The technique is versatile and can be applied to practically any local oscillator at any frequency.

Record 114 of 193

Radiation from Intrinsic Josephson Junctions in Misaligned Tl2Ba2CaCu2O8 Thin Films

Wang, P.; Fan, B.; Wang, Z.; Xie, W.; Zhao, X. J.; Zhang, X.; Ji, L.; He, M.; Fang, L.; Yan, S. L.

JOURNAL OF SUPERCONDUCTIVITY AND NOVEL MAGNETISM

卷: 25; 期: 5; 页: 1427-1430

We measure the current-voltage (I-V) curves of intrinsic Josephson junctions (IJJs) in misaligned Tl2Ba2CaCu2O8

thin films embedded in a Fabry-P,rot (F-P) resonator at liquid nitrogen temperature. Regarding the substrate as a dielectric resonator, electromagnetic coupling between the intrinsic Josephson junctions is improved. By adjusting the location of the substrate in the F-P resonator, the critical current of the IJJs under microwave irradiation (75.6 GHz) is suppressed almost to zero. Two pairs of symmetrical radiation (75.6 GHz) peaks are detected. Possible explanations for this experimental result are discussed.

Record 115 of 193

Terahertz Wavefronts Measured Using the Hartmann Sensor Principle

M. Cui; J. N. Hovenier; Ren, Y.; A. Polo;J. R. Gao

Optics Express

卷: 20; 期: 13; 页: 14380-14391

We demonstrate for the first time that the Hartmann wavefront sensor (HWS) principle can be applied for characterizing the wavefronts of terahertz (THz) electromagnetic radiation. The THz Hartmann wavefront sensor consists of a metallic plate with an array of holes and a two-dimensional scanable pyro-electric detector. The THz radiation with different wavefronts was generated by a far-infrared gas laser operated at 2.5 THz in combination with a number of objects that result in known wavefronts. To measure the wavefront, a beam passing through an array of holes generates intensity spots, for which the positions of the individual spot centroids are measured and compared with reference positions. The reconstructed wavefronts are in good agreement with the model expectations.

Record 116 of 193

Direct Detection of Terahertz Signals at 493GHz Using Nb Superconducting Tunnel Junctions

Wang, Zheng; Dong Liu; Jing Li; Sheng-Cai Shi


卷: 2; 页: 1-4

Superconducting tunnel junctions are good candidates for the direct detection of terahertz signals. In this paper, the direct detection behavior of Nb-based superconducting tunnel junctions at 493GHz is demonstrated. The performance of the detector is evaluated in several aspects, including noise characteristics, current response and frequency response.

Record 117 of 193

Frequency Locking Of Single-Mode 3.5-THz Quantum Cascade Lasers Using a Gas Cell

Ren, Y.; Hovenier, J.N.; Cui, M.; Hayton, D.J.; Gao, J.R.; Klapwijk, T.M.; Shi, S.C.; Kao, T.-Y.; Hu, Q.; Reno, J.L.


53

Applied Physics Letters

卷: 100; 期: 4; 页: 041111-1-041111-4

We report frequency locking of two 3.5-THz third-order distributed feedback (DFB) quantum cascade lasers (QCLs) by using methanol molecular absorption lines, a proportional-integral-derivative controller, and a NbN bolometer. We show that the free-running linewidths of the QCLs are dependent on the electrical and temperature tuning coefficients. For both lasers, the frequency locking induces a similar linewidth reduction factor, whereby the narrowest locked linewidth is below 18 kHz with a Gaussian-like shape. The linewidth reduction factor and the ultimate linewidth correspond to the measured frequency noise power spectral density.

Record 118 of 193

Analysis of Multiport Passive Components Using Admittance Matrix

Miao, Chen; Ge Tian; Yang, JinPing; Wen Wu


卷: 2; 页: 1-4

Based on the network matrix conversion from scatter parameters to admittance parameters, a novel analysis method for multiport passive components is presented. Unlike the traditional even- and odd-mode analysis only being used for symmetrical structure, this kind of method is no limited. In this paper, three examples, such as Wilkinson power divider, 180° ring hybrids and quadrature (90°) hybrids with arbitrary port impedances are researched. Analysis results show that design formulas obtained from new method agree with ones reported by class literatures, but the calculation process is much simpler than class methods obviously.

Record 119 of 193

Frequency and Amplitude Stabilized Terahertz Quantum Cascade Laser as Local Oscillator

Ren, Y.; D.J.Hayton; J.N.Hovenier; M.Cui; J.R.Gao; T.M.Klapwijk; S.C.Shi; T.Y.Kao; Q.hu; L.Reno

APPLIED PHYSICS LETTERS

卷: 101; 期: 10; 页: 101111-1-101111-4

We demonstrate an experimental scheme to simultaneously stabilize the frequency and amplitude of a 3.5 THz third-order distributed feedback quantum cascade laser as a local oscillator. The frequency stabilization has been realized using a methanol absorption line, a power detector, and a proportional-integral-derivative (PID) loop. The amplitude stabilization of the incident power has been achieved using a swing-arm voice coil actuator as a fast optical attenuator, using the direct detection output of a superconducting mixer in combination with a 2nd PID loop. Improved Allan variance times of the entire

receiver, as well as the heterodyne molecular spectra, are demonstrated.

Record 120 of 193

Millimeter-Wave Radiation from Misaligned Tl2Ba 2CaCu2O8 Thin-Film Intrinsic Josephson Junctions

Wang, P.; Wang Zh.; B. Fan; W. Xie; W. Liu; XJ. Zhao; X. Zhang; L. Ji; M. He; L. Fang; S.L. Yan

IEEE Transctions on applied superconductivity

卷: 22; 期: 5; 页: 1500503

We have measured the current-voltage characteristics of misaligned Tl2Ba2CaCu2O8 thin-film intrinsic Josephson junctions (IJJs) embedded in a quasi-optical resonator at 78.5 K. The substrate is regarded as a dielectric resonator to improve high-frequency electromagnetic coupling between the IJJs. The experimental result is fitted well with the electromagnetic simulation. Radiation power larger than 10 pW has been detected at 75.6 GHz. Moreover, the phenomenon of jump voltage is explored, and a possible explanation is discussed.

Record 121 of 193

Twin Slot Antenna Patterns of a Quasi-Optical HEB Mixer at THz Frequencies

Zhou, K.M.; Delorme, Y.; Feret, A.; Miao, W.; Lefevre, R.; Vacelet, T.; Shi, S.C.


卷: 5; 页: 1-3

Results of far-field beam pattern measurements of the 1.25 THz superconducting Hot Electron Bolometer (HEB) mixer on a quasi-optical integrated lens antenna are presented. The integrated antenna consists of a planar twin slot antenna mounted on the flat surface of an extended hemispherical lens. The beam patterns have been measured at three frequencies: 1.35 THz, 1.395 THz and 1.47 THz with a new setup which has a focus lens between source and HEB mixer. The first order side lobe level equals -13 dB. The dynamic range is nearly 30 dB. The simulated result is also presented, it agrees with measured one well.

Record 122 of 193

Research on the Equivalent Circuit of Microstrip T-Junctions and Its Application on Branch-Line Coupler

Tian, Ge; Yang, Jin-Ping; Lan Cui; Wen Wu; Sheng-Cai Shi


卷: 1; 页: 1-4

Analysis of microstrip T-junctions based on their equivalent circuit model is introduced in this paper. Explicit design formulas are derived using the admittance-matrix. Improved T-junctions with convex


54

and concave segments are investigated and applied to the branch-line coupler with center frequency of 12GHz. The return loss of the coupler is better than -36.3 dB in all ports with isolation of -43.8 dB at the center frequency, while the amplitude imbalance is below 0.12 dB.

Record 123 of 193

Temperature-dependent Performances of Nb SIS Mixers at Millimeter and Submillimeter Wavelength Microwave and Millimeter Wave Technology

Liu, Jie; Wenlei Shan; Shengcai Shi

Microwave and Millimeter Wave Technology (ICMMT), 2012 International Conference on

卷: 5; 页: 1-4

The dependence of the performance of Superconductor-Insulator-Superconductor (SIS) mixers on the ambient temperature is investigated both theoretically and experimentally at millimeter and submillimeter wavelength. We found that the mixers' conversion gain plays a dominant role in the temperature-induced variation of the overall receiver sensitivity. To achieve a straightforward image of how the ambient temperature influences the conversion gain, we introduce a pure shape factor that allows for determining the mixers' conversion gain from the nonlinearity of their IV curves. We measured the performance of an SIS mixer at 100GHz band with the ambient temperature ranging from 3.8K to 8.5K to verify the validity of the quantum mixing theory. The experimental results are found in good agreement with the simulation results. This agreement indicates the validity of quantum mixing theory at a relatively high temperature up to the superconducting critical temperature. The measurement results show that at 100GHz band, the Nb SIS mixer can maintain a reasonable performance at the ambient temperature as high as 80% of the superconducting critical temperature. In addition to the gain and noise, the receiver stability in terms of Allen variance was also measured at various ambient temperatures without any apparent difference found.

Record 124 of 193

Development of a 385-500 GHz Sideband-Separating Balanced SIS Mixer

Serizawa, Yasutaka; Sekimoto, Yutaro; Kamikura, Mamoru; Shan, Wenlei; Ito, Tetsuya; Tamura, Tomonori; Noguchi, Takashi

JOURNAL OF INFRARED MILLIMETER AND TERAHERTZ WAVES

卷: 33; 期: 10; 页: 999-1017

A submillimeter (385-500 GHz) low-noise sideband-separating balanced SIS (Superconductor Insulator Superconductor) mixer (Balanced 2SB mixer)

with high IRR (Image Rejection Ratio) has been successfully developed, whose SSB (Single SideBand) noise temperature is similar to 200 K (10hf/k) with an image rejection ratio of a parts per thousand yenaEuro parts per thousand a1/410 dB. Balanced mixers have become a promising technology which would break through the limitation especially in terahertz receivers and heterodyne arrays. However, though there are examples in microwave with relatively worse noise performance, submillimeter and terahertz balanced mixers have rarely been developed in spite of their astronomical importance. The developed balanced 2SB mixer is not only the first one demonstrated at submillimeter frequency range, but also has very low noise, high IRR, wide detectable frequencies (385-500 GHz), and a flat IF output spectrum. The balanced 2SB mixer is composed of three RF hybrids, four DSB (Double SideBand) mixers, two 180A degrees IF hybrids, and an IF quadrature hybrid. Several important performance indicators such as noise temperature, IRR, required LO (Local Oscillator) power, and IF spectra were measured. The measured LO power required for the balanced 2SB mixer was typically similar to 14 dB less than that of the single-ended mixers.

Record 125 of 193

An Effective Method for Improving Emissions from Intrinsic Josephson Junction Arrays of Misaligned Tl2Ba2CaCu2O8+delta Thin Films

Wang, Z.; Fan, B.; Wang, P.; Ji, L.; Zhao, X. J.; Yan, S. L.

JOURNAL OF SUPERCONDUCTIVITY AND NOVEL MAGNETISM

卷: 25; 期: 7; 页: 2259-2263

In this paper, an effective method for improving emissions from Josephson junction arrays was proposed. We took the substrate as a dielectric resonance antenna to improve the coupling of intrinsic junctions to electromagnetic waves. Electromagnetic simulations were performed in parallel with experiment investigations. Sharp radiation peaks at 76.9 GHz were detected from intrinsic Josephson junction arrays in misaligned Tl2Ba2CaCu2O8+delta thin films at 78 K. Experimental results proved the effectiveness of this method, which offered a competitive choice for coherent emission from intrinsic Josephson junction arrays.

Record 126 of 193

Exact De Sitter Solutions in Quadratic Gravitation with Torsion

Chee, Guoying; Guo, Yongxin

CLASSICAL AND QUANTUM GRAVITY

卷: 29; 期: 23; 页: 235022

Several exact cosmological solutions of quadratic gravitation with two torsion functions are presented. These solutions give an essentially different explanation from the one in most of previous works to the cause of


55

the accelerating cosmological expansion and the origin of the torsion of the spacetime. These solutions can be divided into two classes. The solutions in the first class define the critical points of a dynamic system representing an asymptotically stable de Sitter spacetime. The solutions in the second class have exact analytic expressions which have never been found in the literature. The acceleration equation of the universe in general relativity is only a special case of them. These solutions indicate that even in vacuum the spacetime can be endowed with torsion, which means that the torsion of the spacetime has an intrinsic nature and a geometric origin. In these solutions the acceleration of the cosmological expansion is due to either the scalar torsion or the pseudoscalar torsion function. Neither a cosmological constant nor dark energy is needed. It is the torsion of the spacetime that causes the accelerating expansion of the universe in vacuum. All the effects of the inflation, the acceleration and the phase transformation from deceleration to acceleration can be explained by these solutions. Furthermore, the energy and pressure of the matter without spin can produce the torsion of the spacetime and make the expansion of the universe decelerate as well as accelerate.

Record 127 of 193

A Sensitive Survey of Dense Parts of Outflows toward Massive Cores

Sun, Yan; Xu, Ye; Yang, Ji


卷: 53; 期: 2; 页: 97-105

A sample of 13 massive star-forming cores was

observed in SiO（2-1）,CH_3OH（2- 1） and C~(34)S

（ 2-1 ） thermal lines.Nine of these cores were

detected in all three lines.Among the nine SiO detections, three were new detections and were relatively faint.Most of the lines have wide wings, which might be interpreted as the evidence of ongoing energetic outflows in the cores.The line widths of SiO are generally the broadest, which might further suggest that SiO emissions are due to higher velocity outflow and are closer to the excited source. We derive the rotational temperatures, column densities, and chemical relative abundances of the cores.There is a strong correlation between SiO and CH_3OH abundances, with correlation coefficient R = 0.77, but no correlation is observed between SiO and C~(34)S.

Record 128 of 193

Trigonometric Parallaxes of Massive Star-Forming Regions. IX. The Outer Arm in the First Quadrant

Sanna, A.; Reid, M. J.; Dame, T. M.; Menten, K. M.; Brunthaler, A.; Moscadelli, L.; Zheng, X. W.; Xu, Y.


卷: 745; 期: 1; 页: 82-88

We report a trigonometric parallax measurement with the Very Long Baseline Array for the water maser in the distant high-mass star-forming region G75.30+1.32. This source has a heliocentric distance of 9.25(-0.40)(+0.45) kpc, which places it in the Outer arm in the first Galactic quadrant. It lies 200 pc above the Galactic plane and is associated with a substantial H i enhancement at the border of a large molecular cloud. At a Galactocentric radius of 10.7 kpc, G75.30+1.32 is in a region of the Galaxy where the disk is significantly warped toward the North Galactic Pole. While the star-forming region has an instantaneous Galactic orbit that is nearly circular, it displays a significant motion of 18 km s(-1) toward the Galactic plane. The present results, when combined with two previous maser studies in the Outer arm, yield a pitch angle of about 12 degrees for a large section of the arm extending from the first quadrant to the third.

Record 129 of 193

Massive Star Formation toward G28.87+0.07 (IRAS 18411-0338) Investigated By Means Of Maser Kinematics and Radio to Infrared Continuum Observations

Li, J. J.; Moscadelli, L.; Cesaroni, R.; Furuya, R. S.; Xu, Y.; Usuda, T.; Menten, K. M.; Pestalozzi, M.; Elia, D.; Schisano, E.


卷: 749; 期: 1; 页: 47-62

We used the Very Long Baseline Array and the European VLBI Network to perform phase-referenced very long baseline interferometry observations of the three most powerful maser transitions associated with the high-mass star-forming region G28.87 + 0.07: the 22.2 GHz H2O, 6.7 GHz CH3OH, and 1.665 GHz OH lines. We also performed Very Large Array (VLA) observations of the radio continuum emission at 1.3 and 3.6 cm and Subaru observations of the continuum emission at 24.5 mu m. Two centimeter-continuum sources are detected and one of them (named hot molecular core (HMC)) is compact and placed at the center of the observed distribution of H2O, CH3OH, and OH masers. The bipolar distribution of line-of-sight velocities and the pattern of the proper motions suggest that the water masers are driven by a (proto) stellar jet interacting with the dense circumstellar gas. The same jet could both excite the centimeter-continuum source named HMC (interpreted as free-free emission from shocked gas) and power the molecular outflow observed at larger scales-although one cannot exclude that the free-free continuum is rather originating from a hypercompact H II region. At 24.5 mu m, we identify

Qinhai Observation Station


56

two objects separated along the north-south direction, whose absolute positions agree with those of the two VLA continuum sources. We establish that similar to 90% of the luminosity of the region (similar to 2 x 10(5) L-circle dot) is coming from the radio source HMC, which confirms the existence of an embedded massive young stellar object exciting the masers and possibly still undergoing heavy accretion from the surrounding envelope.

Record 130 of 193

A 95 GHz Class I Methanol Maser Survey toward a Sample of Glimpse Point Sources Associated With BGPS Clumps

Chen, Xi; Ellingsen, Simon P.; He, Jin-Hua; Xu, Ye; Gan, Cong-Gui; Shen, Zhi-Qiang; An, Tao; Sun, Yan; Ju, Bing-Gang

ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES

卷: 200; 期: 1; 页: L29-L86

We report a survey with the Purple Mountain Observatory 13.7 m radio telescope for class I methanol masers from the 95 GHz (8(0)-7(1) A(+)) transition. Two hundred and fourteen target sources were selected by combining information from both the Spitzer GLIMPSE and 1.1 mm Bolocam Galactic Plane Survey (BGPS) catalogs. The observed sources satisfy the GLIMPSE mid-IR criteria of [3.6]-[4.5] > 1.3, [3.6]-[5.8] > 2.5, [3.6]-[8.0]> 2.5 and 8.0 mu m mag less than 10; they also have an associated 1.1 mm BGPS source. Class I methanol maser emission was detected in 63 sources, corresponding to a detection rate of 29% for this survey. For the majority of detections (43), this is the first identification of class I methanol masers associated with these sources. We show that the intensity of the class I methanol maser emission is not closely related to mid-IR intensity or the colors of the GLIMPSE point sources; however, it is closely correlated with properties (mass and beam-averaged column density) of the BGPS sources. Comparison of measures of star formation activity for the BGPS sources with and without class I methanol masers indicates that the sources with class I methanol masers usually have higher column density and larger flux density than those without them. Our results predict that the criteria log(S-int) <= -38.0 + 1.72 log(N-H2(beam)) and log(N-H2(beam)) >= 22.1, which utilizes both the integrated flux density (S-int) and beam-averaged column density (N-H2(beam) ) of the BGPS sources, are very efficient for selecting sources likely to have an associated class I methanol maser. Our expectation is that searches using these criteria will detect 90% of the predicted number of class I methanol masers from the full BGPS catalog (similar to 1000), and that they will do so with a high detection efficiency (similar to 75%).

Record 131 of 193

Gas Emissions in Planck Cold Dust Clumps-A Survey of the J=1-0 Transitions of (CO)-C-12, (CO)-C-13, And (CO)-O-18

Wu, Yuefang; Liu, Tie; Meng, Fanyi; Li, Di; Qin, Sheng-Li; Ju, Bing-Gang


卷: 756; 期: 1; 页: 76-99

A survey toward 674 Planck cold clumps of the Early Cold Core Catalogue (ECC) in the J = 1-0 transitions of (CO)-C-12, (CO)-C-13, and (CO)-O-18 has been carried out using the Purple Mountain Observatory 13.7 m telescope. Six hundred seventy-three clumps were detected with (CO)-C-12 and (CO)-C-13 emission, and 68% of the sample has (CO)-O-18 emission. Additional velocity components were also identified. A close consistency of the three line peak velocities was revealed for the first time. Kinematic distances are given for all the velocity components, and half of the clumps are located within 0.5 and 1.5 kpc. Excitation temperatures range from 4 to 27 K, slightly larger than those of T-d. Line width analysis shows that the majority of ECC clumps are low-mass clumps. Column densities N-H2 span from 10(20) to 4.5 x 10(22) cm(-2) with an average value of (4.4 +/- 3.6) x 10(21) cm(-2). N-H2 cumulative fraction distribution deviates from the lognormal distribution, which is attributed to optical depth. The average abundance ratio of the (CO)-C-13 to (CO)-O-18 in these clumps is 7.0 +/- 3.8, higher than the terrestrial value. Dust and gas are well coupled in 95% of the clumps. Blue profile asymmetry, red profile asymmetry, and total line asymmetry were found in less than 10% of the clumps, generally indicating that star formation is not yet developed. Ten clumps were mapped. Twelve velocity components and 22 cores were obtained. Their morphologies include extended diffuse, dense, isolated, cometary, and filament, of which the last is the majority. Twenty cores are starless, and only seven cores seem to be in a gravitationally bound state. Planck cold clumps are the most quiescent among the samples of weak red IRAS, infrared dark clouds, UC H II candidates, extended green objects, and methanol maser sources, suggesting that Planck cold clumps have expanded the horizon of cold astronomy.

Record 132 of 193

Trigonometric Parallax of RCW 122

Wu, Y. W.; Xu, Y.; Menten, K. M.; Zheng, X. W.; Reid, M. J.

Cosmic Masers - from OH to H0, Proceedings of the International Astronomical Union, IAU Symposium

卷: 287; 页: 425-426

As a part of the BeSSeL (Bar and Spiral Structure Legacy) survey, we report a trigonometric parallax for the massive star-forming region G348.70-1.04. Its distance is 3.38-0.27 +0.33 kpc, indicating that it is in the Scutum-Centaurus arm. Its proper motion is -0.73 +/- 0.04 mas yr-1 toward the east and -2.83 +/- 0.50 mas yr-1 toward the north.


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Record 133 of 193

Massive Star-Formation toward G28.87+0.07

Li, JJ; Moscadelli, L; Cesaroni, R; Furuya, RS; Xu, Y; Usuda, T; Menten, KM; Pestalozzi, M; Elia, D; Schisano, E

Solar and Stellar Astrophysics

卷: 749; 期: 1; 页: 47

We used the Very Long Baseline Array (VLBA) and the European VLBI Network (EVN) to perform phase-referenced VLBI observations of the three most powerful maser transitions associated with the high-mass star-forming region G28.87+0.07: the 22.2 GHz H$_{2}$O, 6.7 GHz CH$_{3}$OH, and 1.665 GHz OH lines. We also performed VLA observations of the radio continuum emission at 1.3 and 3.6 cm and Subaru observations of the continuum emission at 24.5 $\mu$m. Two centimeter continuum sources are detected and one of them (named "HMC") is compact and placed at the center of the observed distribution of H$_{2}$O, CH$_{3}$OH and OH masers. The bipolar distribution of line-of-sight (l.o.s) velocities and the pattern of the proper motions suggest that the water masers are driven by a (proto)stellar jet interacting with the dense circumstellar gas. The same jet could both excite the centimeter continuum source named "HMC" (interpreted as free-free emission from shocked gas) and power the molecular outflow observed at larger scales -- although one cannot exclude that the free-free continuum is rather originating from a hypercompact \ion{H}{2} region. At 24.5 $\mu$m, we identify two

objects separated along the north-south direction, whose absolute positions agree with those of the two VLA continuum sources. We establish that $\sim$90% of the luminosity of the region ($\sim$\times10^{5} L_\sun$) is coming from the radio source "HMC", which confirms the existence of an embedded massive young stellar object (MYSO) exciting the masers and possibly still undergoing heavy accretion from the surrounding envelope.

Record 134 of 193

Methanol Maser Parallaxes and Proper Motions

Xu, Y.; Reid, M. J.; Moscadelli, L.; Menten, K. M.; Zheng, X. W.; Brunthaler, A.; Zhang, B.; Rygl, K. L. J.; Li, J. J.; Sanna, A.

Cosmic Masers - from OH to H0, Proceedings of the International Astronomical Union, IAU Symposium

卷: 287; 页: 368-376

Due to their compactness, persistence and slow motion, Class II CH3OH masers are excellent targets for parallax and proper motion measurements for massive star-forming regions in the Galactic Disk. These measurements can be used to improve our understanding of the spiral structure and dynamics of the Milky Way. At the same time, Class II CH3OH masers can also be used to study gas kinematics close to the exciting star, tracing rotation, infall and/or outflow motions.


58

III. Applied Celestial Mechanics and Space Object & Debris Research

Record 135 of 193

Use of Mathematic Morphological Operators for Processing the Smeared Images of a Camera without Shutter

Sun, Rong-yu; Zhao, Chang-yin; Ping, Yi-ding; Xiong, Jian-ning; Zhang, Chen


卷: 36; 期: 3; 页: 340-352

In the observation of space objects with a full-frame transfer CCDcamera, the camera shutter is often removed, and therefore the smearedimages are produced, which affect seriously the object detection and location. Based on the difference of geometrical morphology between starimages and smears, a mathematical morphology method is proposed to process the smeared images. By comparing the position accuracies of stars and space objects before and after processing, it is verified that the morphological method can effectively remove the smears from astronomical images, and can significantly improve the detection rates and position accuracies of stars and moving objects. The result indicates that this is an effective method to eliminate the smearing effect.

Record 136 of 193

A New Approach to the Electro-optical Tracking of a Space Object

Wang, Xin; Xu, Zhanwei


卷: 53; 期: 2; 页: 145-152

The electro-optical tracking of the space object is often interrupted by the dropped frames caused by the occlusion of stars.In this paper,two stages of the tracking process,predicting as well as sampling,are studied in the probabilitic point of view.Base on the theory of estimation,a new method is proposed by employing the Kalman filter for robust predicting due to the characteristic of the data fusion,and the mean shift process for the adjustment of the tracking window.Corresponding experiment shows that the method can effectively reduce the impact of interference,and improve the robustness during the tracking process.

Record 137 of 193

Assignment of Space Objects for Electro-Optical Observation Network

Wang, Xin

Journal of Spacecraft TT&C Technology

卷: 31; 期: 6; 页: 86-89

To meet requirements of assignment of space objects to equipment in an observation network, a concept of catalog efficiency is proposed together with a computing algorithm, taking into concideration detection ratio, data pattern for catalog orbit determination and update frequency. Based on the concept, a linear programming model is constructed for space object assignment optimization. Numerical simulation shows that the model is effective and can be used in operation of an obervation network to increase efficiency. The concept of catalog efficiency can also be taken as a measurement of the cost of observation resource in evaluation of the catalog ability of an obseration network.

Record 138 of 193

A Definite Integration Method of Calculating Inclination Function and its Derivative

Wu, Lianda; Wang, Hongbo


卷: 53; 期: 1; 页: 51-61

The paper gives a definite integration method of calculating inclination function and its derivative.The expression is simple,but its accuracy is very well.It is about 10-15 and 10-13 for inclination function and its derivative,respectively.This level is comparable to the accuracy of Goodings method.Through a lot of numerical simulations,it is proved that the method has good stability and wide-scope application of inclination.It takes very little time to calculate low-order

function（less than 50）,so the method can be directly

used in calculating terrestrial and sun-moon gravitational perturbation.

Record 139 of 193

An Automatic Identification Method for GEO Space Objects

Sun, Rongyu; Zhao, Changyin

Journal of Spacecraft TT&C Technology

卷: 31; 期: 6; 页: 90-94

Center for Space Object and Debris

Research


59

It is difficult to detect and track GEO (Geostationary Earth Orbit) objects automatically using only two short exposure time frames with different method due to the relatively slow velocity between background stars and GEO space objects. A technique based upon Lucas-Kanade algorithm is presented to resolve this problem. First, specific gates are set around all star images on the frame. Then, the moving velocity of all gates is obtained. Finally, the GEO objects are identified according to the specific movement fearures using the global statistical threshold. Simulation and tests demonstrate that the method works effectively with robust performance. The displacement precision of object images is about 10

-3 and the computing time is

less than 0.1s, showing a high value for realtime data processing.

Record 140 of 193

Optical Survey Technique for Space Debris in GEO

Sun, Rongyu; Zhao, Changyin


卷: 30; 期: 3; 页: 394-410

In view of the special dynamical characteristics of geosynchronous orbits, the GEO ring is a unique environment for application. However, in this region there is no natural removal mechanism for space debris, which has been recognized as an increasing threat for space operations. Concerning the short detection distance of ground-based radar, ground-based optical survey is the major technique for observing space debris in GEO. The survey techniques for space debris observation are introduced in detail, including

specialized hardware、survey strategy proposed and

advanced image processing algorithm. Several algorithms are summarized for separating the blended images in optical space debris observation and removing the smear noise in images of camera without shutter, they all work effectively and robustly. Discussions are made in high order precision positioning methods for space debris, and futhermore the development of these methods is outlooked. For enriching the space debris situation in GEO, and protecting the security of active space operations, the technique for optical survey of space debris in GEO should be further studied.

Record 141 of 193

Two Methods for Deriving the Recursion Formula of Inclination Function



卷: 53; 期: 5; 页: 402-410

In analytical theories of celestial mechanics,the perturbation function need be expanded as a function of orbit elements.There are two frequently-used

functions.One is the inclination function,another is the Hansen coefficient.How to calculate the inclination function as well as its stability and accuracy are very elementary and important problems in satellite dynamics.The method for deriving the recursion formula of Goodings inclination function is based on two hyper-geometric series relations.Then it is proved that the Gooding formula can also be deduced by the recursion relation of Jacobi polynomial.Comparing with the hyper-geometric series,the recursion process based on Jacobi polynomial is much simpler,indicating that the Gooding method is the recursion of Jacobi polynomial in essence.

Record 142 of 193

A New Approach to the Electro-optical Tracking of a Space Object

Wang, Xin; Xu, Zhanwei


卷: 53; 期: 2; 页: 145-152

The electro-optical tracking of the space object is often interrupted by the dropped frames caused by the occlusion of stars.In this paper,two stages of the tracking process,predicting as well as sampling,are studied in the probabilitic point of view.Base on the theory of estimation,a new method is proposed by employing the Kalman filter for robust predicting due to the characteristic of the data fusion,and the mean shift process for the adjustment of the tracking window.Corresponding experiment shows that the method can effectively reduce the impact of interference,and improve the robustness during the tracking process.

Record 143 of 193

On The Triangular Libration Points in Photogravitational Restricted Three-Body Problem with Variable Mass

Zhang, Ming-Jiang; Zhao, Chang-Yin; Xiong, Yong-Qing


卷: 337; 期: 1; 页: 107-113

This paper investigates the triangular libration points in the photogravitational restricted three-body problem of variable mass, in which both the attracting bodies are radiating as well and the infinitesimal body vary its mass with time according to Jeans' law. Firstly, applying the space-time transformation of Meshcherskii in the special case when q=1/2, k=0, n=1, the differential equations of motion of the problem are given. Secondly, in analogy to corresponding problem with constant mass, the positions of analogous triangular libration points are obtained, and the fact that these triangular libration points cease to be classical ones when alpha not equal 0, but turn to classical L (4) and L (5) naturally when alpha=0 is pointed out. Lastly, introducing the


60

space-time inverse transformation of Meshcherskii, the linear stability of triangular libration points is tested when alpha > 0. It is seen that the motion around the triangular libration points become unstable in general when the problem with constant mass evolves into the problem with decreasing mass.

Record 144 of 193

Using Operators of Morphological Mathematic for Processing Smeared Image of Camera without Shutter

Sun, Rongyu; Zhao, Changyin; Ping, Yiding; Xiong, Jianning; Zhang, Chen


卷: 53; 期: 1; 页: 80-91

In observations of space objects,the shutter of camera is often removed and hence the smear noise is ineluctable.Smear noise brings in difficulties on target detection and location calculation,so it must be handled properly.Based on the differences of geometry between stars and smear noise,two operators(TopHat and Spread TopHat) of morphological mathematic are presented to resolve this problem.Theyre sufficiently flexible to be applied.Tests carried out indicate that smear noise can be removed effectively,and detection rate of objects and stars is improved distinctly.Through the compare of position accuracy of stars and objects,its demonstrated that both two operators work with a high degree of location precision,and Spread TopHat has a better performance when dealing with stars.At last,the efficiency of methods is proved.

Record 145 of 193

A Definite Integration Method of Calculating Inclination Function and its Derivative



卷: 53; 期: 1; 页: 51-61

The paper gives a definite integration method of calculating inclination function and its derivative.The expression is simple,but its accuracy is very well.It is about 10-15 and 10-13 for inclination function and its derivative,respectively.This level is comparable to the accuracy of Goodings method.Through a lot of numerical simulations,it is proved that the method has good stability and wide-scope application of inclination.It takes very little time to calculate low-order

function（less than 50）,so the method can be directly

used in calculating terrestrial and sun-moon gravitational perturbation.

Record 146 of 193

A New Method for Detecting GEO Space Objects with Image Stacking

Sun, Rongyu; Ping, Yiding; Zhao, Changyin


卷: 53; 期: 3; 页: 249-258

To meet the needs of detecting GEO(Geosynchronous Orbit)space objects, and prevent the saturation of CCD pixels with long exposure time,a method of stacking series of images with short exposure time is presented.Using the method,the store range of images is enlarged,and the signal to noise ratio(SNR)is promoted,and hence the detection ability of the whole system is improved.The results of experiments demonstrate that the saturation of pixels is eliminated effectively,and the SNR is increased by 3.2 times,and the detection ability is increased by 2.5 magnitude when 10 seriate images are stacked.The location accuracy of stars satisfies the requirement,and using the mean plate parameters for astronomical orientation is reliable.At last the efficiency of the method is proved.

Record 147 of 193

Low-thrust Trajectory Optimization Using Indirect Shooting Method without Initial Costate Guess

Lin, Houyuan; Zhao, Changyin


卷: 53; 期: 3; 页: 197-204

Based on the optimal control theory,the optimal control problem of the lowthrust trajectory is transformed into a sequence of nonlinear two-point bound-value problem (TPBVP).In the process of solving the TPVBP,the initial constates need repeated random guesses and iterative computations.In order to enhance the convergence of the iteration, we select an appropriate performance index,and then linearize the equations of the TPBVP around the Keplerian orbits.For multi-revolution transfers,we use the multi-splicing Keplerian arcs instead of the multi-revolution Lambert trajectory to ensure the effectiveness of the linearization.The method is totally automatic with multiple iterations.With this method,we can get the results within 3 ~ 5 iterations,and the random guess of the initial constates is unnecessary.Then by iterative optimization of the performance index,we can get a better control strategy.

Record 148 of 193

Mei Symmetry of Discrete Mechanico-Electrical Systems

Zhang, M. J.

ACTA MECHANICA

卷: 223; 期: 4; 页: 679-683

Mei symmetry of discrete mechanico-electrical systems on a uniform lattice is investigated. The definition and criterion of the discrete analog of Mei symmetry for the system are presented. The condition of existence of the discrete Mei conserved quantity induced directly by Mei


61

symmetry as well as its form is given. Finally, an example is discussed to illustrate these results.

Record 149 of 193

Perturbation to Noether Symmetry and Noether Adiabatic Invariants of Discrete Difference Variational Hamilton Systems

Zhang, M. -J.; Fang, J. -H.

ACTA PHYSICA POLONICA A

卷: 122; 期: 1; 页: 25-30

The perturbation to the Noether symmetry and the Noether adiabatic invariants of discrete difference variational Hamilton systems are investigated. The discrete the Noether exact invariant induced directly by the the Noether symmetry of the system without perturbation is given. The concept of discrete high-order adiabatic invariant is presented, the criterion of the perturbation to the Noether symmetry is established, and the discrete the Noether adiabatic invariant induced directly by the perturbation to the Noether symmetry is obtained. Lastly, an example is discussed to illustrate the application of the results.

Record 150 of 193

Reply To: "Comment On The Paper 'On The Triangular Libration Points In Photogravitational Restricted Three-Body Problem With Variable Mass'" By Varvoglis, H. and Hadjidemetriou, J.D.

Zhang, Ming-Jiang


卷: 340; 期: 2; 页: 209-210

Recently Varvoglis and Hadjidemetriou (Astrophys. Space Sci. doi: 10.1007/s10509-012-1060-3, 2012; hereafter referred to as paper VH) have raised two points concerning the model of the restricted three-body problem with variable mass presented in our paper (Zhang et al. in Astrophys. Space Sci. 337:107, 2012; hereafter referred to as paper ZZX) and made intensive investigations of this model. These points and investigations are very useful and here we provide some explanation and supplementary specification regarding the model presented in the paper ZZX.

Record 151 of 193

A Method of Separating Blended Images in Space Debris Observation

Sun, RongYu; Zhao, ChangYin; Zhang, YiPing


卷: 55; 期: 10; 页: 1945-1951

Due to the relative movement between space debris and background stars, the blending of objects and stars is ineluctable through observation. It brings down position accuracy of objects and even makes the tracking break down in worse conditions. In view of the

difference of geometry between stars and objects in space debris observation, a technique for separating blended objects based on mathematical morphology is presented. It's sufficiently flexible to be applied in image processing, and the blending images can be separated effectively with a high degree of centroid precision.

Record 152 of 193

A High Speed Data Transmission System Based on Optic Fiber and PCI Bus

Kou Chaoyong; Liu Wei; Men Jinrui

Optical Communication Technology

卷: 36; 期: 5; 页: 45-47

The data transmission stably is the main bottleneck in the field of huge amount of data, high rate of data and remote distance data transmission. This paper introduces a data transmission system based on optical fiber communication and the PCI bus. The system transmits a large volume data through the optical fiber to the computer, and the data can be displayed and processed in the computer. It is tested that the systems data transmission rate is fast and has far transmission distance and strong anti-interference ability. In addition, this system can be applied to a plurality of systems that need high rate data acquisition and transmission.

Record 153 of 193

Design of CCD Camera Based on Gigabit Ethernet

Men Jinrui; Yao Dazhi; Wei Wei

Laser & Optoelectronics Progress

卷: 49; 期: 3; 页: 0322031-0322035

Domestic science-grade CCD camera generally uses USB 2.0 and its transmission speed is low. Thus, transmission distance is relatively short. In this paper, a CCD camera based on gigabit ethernet interface is designed. A NIOS II soft core system is established by using Altera Company's FPGA (Cyclone II series) as the control system, and a gigabit ethernet transmission system by using the physical layer chip and data link layer chip structure. The transmission speed of the system is up to 700 Mbit/s, and the transmission distance is up to 50 m, so the existing two problems of CCD camera can be overcome.

Record 154 of 193

Laboratory for CCD Camera

Development


62

The ROI Image Abstraction Technology of 1 k×1 k CCD Camera

Liu, Wei; Wei Wei

OPTOELECTRONIC TECHNOLOGY

卷: 32; 期: 2; 页: 123-137

An integral CCD camera system with ROI ( region of interesting) function was developed successfully with KAF-1001 CCD chip. Timing of Pixel driving, AD conversion, data latch were written with CPLD device. The result was simulated. The communication mode of the camera is USB2.0. The paper showed the capture interface and collected ROI pictures to confirm the correctness and reliability of the timing.

Record 155 of 193

Application of Numerical Integration and Data Fusion in Unit Vector Method

Zhang, Jing


卷: 53; 期: 1; 页: 94-95

The Unit Vector Method (UVM) is a series of orbit determination methods which are designed by Purple Mountain Observatory (PMO) and have been applied

extensively. Itgets the conditional equations for different kinds of data by projecting the basic equation to different unit vectors, and it suits ofr weighted process for different kinds of data. The high-precisiion data can play a major role in orbit determination, and accuracy of orbit determination is improved obviously.

Record 156 of 193

The Study and Applications of Satellite and Satellite Constellation Autonomous Orbit Determination Using Star Sensor

Gan, Qingbo


卷: 53; 期: 4; 页: 355-356

Automomous satellite orbit determination is a key technique in autonomous satellite navigation. Many kinds of technologies have been proposed to realize the autonomous satellite navigation, such as the star sensor, the Earth magnetometer, the occultation time survey, and the phase measurement of X-ray pulsar signals.

This dissertation studies a method of autonomous satellite orbit determination using star sensor. Moreover, the method is extended to the autonomous navigation of datellite constellation and the space-based surveillance.

In chapters 1 and 2, some usual time and reference systems are introduced. Then the principles of several typical autonomous navigation methods, and their merits and shortcomings are analyzed…

IV. Planetary Sciences and Deep Space Exploration

Record 157 of 193

Activity of Comet 103P/Hartley 2 from September 30 to November 04, 2010

Shi, JianChun; Zhao, HaiBin; Ma, YueHua


卷: 55; 期: 8; 页: 1515-1518

The CCD photometric observation of comet 103P/Hartley 2 with broadband optical filters was carried out at Xuyi Station of Purple Mountain Observatory, Chinese Academy of Sciences by use of Near Earth Object Telescope (NEOT). We monitored the comet from September 30 to November 4, 2010 and investigated the variation of activities. The Af rho parameter derived from our r broadband data varies

from 46.0 to 126.0 cm and increases with time. The dust production rate in terms of Af rho was measured and a tentative calculation of the dust (or gas) loss-rate of nucleus was executed under the assumption that the nucleus of comet 103P/Hartley 2 is spherical. The r-band image and the surface brightness profile taken on September 30, 2010 was measured and the gradient of surface brightness profile of 103P/Hartley 2 showed m < -1.5.

Record 158 of 193

Numerical Simulation of Time Delay Interferometry for a LISA-like Mission with the Simplification of Having Only One Interferometer

S.V.Dhurandhar; Wei-Tou Ni; Wang, Gang

ADVANCES IN SPACE RESEARCH

卷: 51; 期: 1; 页: 198-206

In order to attain the requisite sensitivity for LISA, laser frequency noise must be suppressed below the secondary noises such as the optical path noise,

Precise Orbit Determination of

Spacecraft

Near Earth Object Survey and Solar

System Bodies

http://english.pmo.cas.cn/rh/dcm/pods/

http://english.pmo.cas.cn/rh/dcm/pods/


63

acceleration noise etc. In a previous paper (Dhurandhar, S.V., Nayak, K.R., Vinet, J.-Y. Time delay interferometry for LISA with one arm dysfunctional. Class. Quantum Grav. 27, 135013, 2010), we have found a large family of second-generation analytic solutions of time delay interferometry with one arm dysfunctional, and we also estimated the laser noise due to residual time-delay semi-analytically from orbit perturbations due to Earth. Since other planets and solar-system bodies also perturb the orbits of LISA spacecraft and affect the time delay interferometry (TDI), we simulate the time delay numerically in this paper for all solutions with the generation number n ⩽ 3. We have worked out a set of 3-year optimized mission orbits of LISA spacecraft starting at January 1, 2021 using the CGC2.7 ephemeris framework. We then use this numerical solution to calculate the residual optical path differences in the second-generation solutions of our previous paper, and compare with the semi-analytic error estimate. The accuracy of this calculation is better than 1 cm (or 30 ps). The maximum path length difference, for all configuration calculated, is below 1 m (3 ns). This is well below the limit under which the laser frequency noise is required to be suppressed. The numerical simulation in this paper can be applied to other space-borne interferometers for gravitational wave detection with the simplification of having only one interferome.

Record 159 of 193

Astrodynamical Space Test of Relativity Using Optical Devices I (ASTROD I)-a Class-M Fundamental Physics Mission Proposal for Cosmic Vision 2015-2025: 2010 Update

Braxmaier, Claus; Dittus, Hansjoerg; Foulon, Bernard; Goeklue, Ertan; Grimani, Catia; Guo, Jian; Herrmann, Sven; Laemmerzahl, Claus; Ni, Wei-Tou; Peters, Achim; Rievers, Benny; Samain, Etienne; Selig, Hanns; Shaul, Diana; Svehla, Drazen; Touboul, Pierre; Wang, Gang; Wu, An-Ming; Zakharov, Alexander F.

EXPERIMENTAL ASTRONOMY

卷: 34; 期: 2; 页: 181-201

ASTROD I is a planned interplanetary space mission with multiple goals. The primary aims are: to test General Relativity with an improvement in sensitivity of over 3 orders of magnitude, improving our understanding of gravity and aiding the development of a new quantum gravity theory; to measure key solar system parameters with increased accuracy, advancing solar physics and our knowledge of the solar system; and to measure the time rate of change of the gravitational constant with an order of magnitude improvement and the anomalous Pioneer acceleration, thereby probing dark matter and dark energy gravitationally. It is envisaged as the first in a series of ASTROD missions. ASTROD I will consist of one spacecraft carrying a telescope, four lasers, two event timers and a clock. Two-way, two-wavelength laser pulse ranging will be used between the spacecraft in a solar orbit and deep space

laser stations on Earth, to achieve the ASTROD I goals.For this mission, accurate pulse timing with an ultra-stable clock, and a drag-free spacecraft with reliable inertial sensor are required. T2L2 has demonstrated the required accurate pulse timing; rubidium clock on board Galileo has mostly demonstrated the required clock stability; the accelerometer on board GOCE has paved the way for achieving the reliable inertial sensor; the demonstration of LISA Pathfinder will provide an excellent platform for the implementation of the ASTROD I drag-free spacecraft. These European activities comprise the pillars for building up the mission and make the technologies needed ready. A second mission, ASTROD or ASTROD-GW (depending on the results of ASTROD I), is envisaged as a three-spacecraft mission which, in the case of ASTROD, would test General Relativity to one part per billion, enable detection of solar g-modes, measure the solar Lense-Thirring effect to 10 parts per million, and probe gravitational waves at frequencies below the LISA bandwidth, or in the case of ASTROD-GW, would be dedicated to probe gravitational waves at frequencies below the LISA bandwidth to 100 nHz and to detect solar g-mode oscillations. In the third phase (Super-ASTROD), larger orbits could be implemented to map the outer solar system and to probe primordial gravitational-waves at frequencies below the ASTROD bandwidth. This paper on ASTROD I is based on our 2010 proposal submitted for the ESA call for class-M mission proposals, and is a sequel and an update to our previous paper (Appouchaux et al., Exp Astron 23:491-527, 2009; designated as Paper I) which was based on our last proposal submitted for the 2007 ESA call. In this paper, we present our orbit selection with one Venus swing-by together with orbit simulation. In Paper I, our orbit choice is with two Venus swing-bys. The present choice takes shorter time (about 250 days) to reach the opposite side of the Sun. We also present a preliminary design of the optical bench, and elaborate on the solar physics goals with the radiation monitor payload. We discuss telescope size, trade-offs of drag-free sensitivities, thermal issues and present an outlook.

Record 160 of 193

Binary Orbit Determination by Using a Variety of Observational Data

Ren Shulin


卷: 53; 期: 3; 页: 261-262

The binary orbit determination is a basic research area

Ephemerial Astronomy and Astronomical

Reference System


64

in astronomy, its main products are the kinematical parmeters of binary, which contain the kinematical parameters of the mass center and the orbital parameters. These parameters are the necessary constituents of the astronomical reference frame with high precision and high density, and at the same time they provide a necessary kinematic basis to the studies of various observed phenomena of binaries. On the other hand, because the binary orbit determination is the only direct route to obtain the stellar masses, which is one of the most fundamental parameters in astronomy, it has received great attention from astronomers for a long time.

Record 161 of 193

The Transformation between Tau and TCB for Deep Space Missions under IAU Resolutions

Deng, Xue-Mei


卷: 12; 期: 6; 页: 703-712

For tracking spacecraft and performing radio science, the transformation between the proper rime (tau) given by a clock carried onboard a spacecraft and the barycentric coordinate time (TCB) is investigated under IAU resolutions. In order to more clearly demonstrate manifestations of a physical model and improve computational efficiency, an analytic approach is adopted. After numerical verification, it is confirmed that this method is adequate to describe a Mars orbiter during one year, and is particularly good at describing the influence from perturbing bodies. Further analyses demonstrate that there are two main effects in the transformation: the gravitational field of the Sun and the velocity of the spacecraft in the barycentric coordinate reference system. The combined contribution of these effects is at the level of a few sub-seconds.

Record 162 of 193

Two-post-Newtonian Light Propagation in The Scalar-Tensor Theory: An N-Point Mass Case

Deng, Xue-Mei; Xie, Yi

PHYSICAL REVIEW D

卷: 86; 期: 4; 页: 044007-1-044007-17

Within the framework of the scalar-tensor theory, its second post-Newtonian (2PN) approximation is obtained with Chandrasekhar's approach. By focusing on an N-point mass system as the first step, we reduce the metric to its 2PN form for light propagation. Unlike previous works, at 2PN order, we abandon the hierarchized hypothesis and do not assume two parametrized post-Newtonian parameters gamma and beta to be unity. We find that although there exist gamma and beta in the 2PN metric, only gamma appears in the 2PN equations of light. As a simple

example for applications, a gauge-invariant angle between the directions of two incoming photons for a differential measurement is investigated after the light trajectory is solved in a static and spherically symmetric spacetime. It shows the deviation from the general relativity delta theta(STT) does not depend on beta even at 2PN level in this circumstance, which is consistent with previous results. A more complicated application is light deflection in a 2-point mass system. We consider a case that the light propagation time is much less than the time scale of its orbital motion and thus treat it as a static system. The 2-body effect at 2PN level originating from relaxing the hierarchized hypothesis is calculated. Our analysis shows the 2PN 2-body effect in the Solar System is one order of magnitude less than future similar to 1 nano-arcsecond experiments, while this effect could be comparable with first post-Newtonian component of delta theta(STT) in a binary system with two Sun-like stars and separation by similar to 0.1 AU if an experiment would be able to measure gamma - 1 down to similar to 10(-6).

Record 163 of 193

The Nonlinear Wave-Wave Interaction of the Kinetic Alfvdn Wave and Its Application in the Solar-Terrestrial Space Plasmas

ZHAO, Jin-song


卷: 53; 期: 5; 页: 451-452

Kinetic Alfvén waves (KAWs) are dispersive Alfvén waves with perpendicular wavelengths comparable to the ion gyroradius or the electron inertial length. The KAWs can play an impotant role in plasma heating, particle acceleration, and anomalous particle transport, and have been extensively applied to carious astrophysical and space plasmas have been an interesting subject with extensive attentions. In this thesis wei study in depth nonlinear wave-wave interaction processes of the KAWs in various plasma environments, and focus on the nonlinear growth rates of the KAWs caused by these wave-wave coupling processes…

Record 164 of 193

Electron Cyclotron Maser Instability in Space Plasmas with Kappa Loss-Cone Distribution

Tang, J. F.; Wu, D. J.; Yan, Y. H.


卷: 745; 期: 2; 页: 134-138

It is well known that non-thermal electrons, often

The Sun and Solar System Plasmas


65

modeled by the kappa distribution, are ubiquitously observed in space. Kappa-type distributions have been widely discussed in various plasma environments. On the other hand, when these non-thermal electrons are trapped by magnetic fields in space they frequently have a loss-cone distribution in velocity space. In this paper, we investigated the growth rates of electron cyclotron maser (ECM) instability in space plasmas by using a kappa loss-cone distribution. Based on the cold plasma assumption and weakly relativistic approximation, the results show that non-thermal electrons with such a distribution can excite ECM emission efficiently. The growth rates of O1 and X2 modes both increase with the kappa spectral index (kappa) but the growth rate of X2 mode increases slightly more rapidly than that of O1 mode. The present analysis also shows that the growth rates increase rapidly with the loss-cone index sigma for sigma < 10 but increase comparatively slowly for larger sigma values.

Record 165 of 193

Alfvenic Turbulence Generated By a Beam of Energetic Ions via Spontaneous Process

Wu, D. J.; Chen, L.; Wu, C. S.

PHYSICS OF PLASMAS

卷: 19; 期: 2; 页: 024511-1-024511-3

Turbulent Alfven waves exist ubiquitously in space and astrophysical plasmas. They may be generated by many different source mechanisms. Among them, ion beam instability is well known. Almost all instability theories are interested in the discussion whether a perturbation will grow or be damped in a given unperturbed state. Few papers elaborate the meaning of growth or amplification in terms of the initial condition. This brief communication complements the existing discussions by considering the effect of spontaneous generation of the waves. In the present study, we estimate the level of spectral energy of Alfvenic turbulence due to the presence of a beam of energetic ions. It is found that the spectral energy may be much higher than the average kinetic energy of the background plasma particles.

Record 166 of 193

Effects of Power-Law Spectrum Behaviors of Nonthermal Electrons on a Ring-Beam Maser Instability

Tang, JianFei; Wu, DeJin; Yan, YiHua


卷: 55; 期: 4; 页: 744-750

The electron-cyclotron maser (ECM) emission driven by nonthermal electrons is one of the most crucial mechanisms responsible for radio emissions in magnetized planets, for the interplanetary medium

(IPM) and for the laboratory microwave generation devices. Major astrophysical observations demonstrate that nonthermal electrons frequently have a negative power-law spectrum with a lower energy cutoff and anisotropic distribution in the velocity space. In this paper, the effects of power-law spectrum behaviors of electrons on a ring-beam maser emission are considered. The results show that the growth rates of O1 and X2 modes decrease rapidly for small Delta (the dispersion of momentum u). Because of the lower energy cutoff behavior, the nonthermal electrons with large Delta still can excite the ECM instability efficiently. The present analysis also includes the effects of parameter beta (beta u (0) is the dispersion of perpendicular momentum u (aSyen), u (0) the average value of u) on the instability. The growth rate of X2 mode decreases with parameter nu (0) (nu (0) = u (aSyen0)/u (0), u (aSyen0) is the average value of u (aSyen)). But for O1 mode, the relationship between the growth rate and nu (0) is complicated. It also shows that the growth rates are very sensitive to frequency ratio Omega (frequency ratio of electron cyclotron frequency to plasma frequency).

Record 167 of 193

Euler Potentials' Discontinuity In The Presence Of Field Line-Aligned Currents

Huang, TianSen; Wu, DeJin


卷: 57; 期: 12; 页: 1436-1437

Since their use in the study of charged particle motion in the 1960s, Euler potentials (alpha, beta) have been widely employed as magnetic field coordinates in both space plasma and fusion plasma studies. People related them to magnetic vector potential A via the relation A = alpha del beta subject to gauge condition A . B = 0 (B is the magnetic induction). For a given magnetic field, the Euler potentials are often constructed with the relation B . Delta S = Delta alpha Delta beta on a surface that crosses the field lines, where Delta S is the area-element surrounding by two line-elements corresponding to the changes in alpha and beta, then mapping the values of alpha and beta along field lines into space. In this short paper, we show that in the presence of field line-aligned currents, the mapping does not work and the orthogonality gauge condition is not satisfied.

Record 168 of 193

The Evidence for the Evolution of Interplanetary Small Flux Ropes: Boundary Layers

Feng HengQiang; Wang JieMin; Wu DeJin



66

卷: 57; 期: 12; 页: 1415-1420

We have examined the Wind data in 1996 and identified 21 small interplanetary magnetic flux ropes (SIMFRs), and all the 21 SIMFRs have boundary layer structures. The durations of the boundary layers varied from several minutes to 30 minutes. These boundary layers also have properties of high proton temperature, density, and plasma beta. These boundary layers are formed by magnetic reconnections. In addition, in three events magnetic reconnections were occurring inside the boundary layers. It indicates that the flux rope structures have propagated for some period of time, and their boundaries were still evolving through interaction with the background solar wind. Namely it is very possible that the SIMFRs came from the solar corona.

Record 169 of 193

On Theories of Solar Type III Radio Bursts

Wu, ChingSheng


卷: 57; 期: 12; 页: 1357-1361

In solar radiophysics, many theories for type Ill bursts have been proposed during the past 60 years. Almost all these theories are based on the plasma hypothesis, which assumes that (i) the radiation is mainly generated by Langmuir waves via nonlinear processes and (ii) the radiation has frequencies close to the local plasma frequency and/or its second harmonic in the source region. We feel strongly that it is time to advocate an alternative approach without recourse to the plasma hypothesis. This brief discussion explains why.

Record 170 of 193

Basic Plasma Processes in Solar-Terrestrial Activities

Wu DeJin; Feng HengQiang


卷: 57; 期: 12; 页: 1353-1356

Within the known universe, more than 99% of all observable matter is plasma, a state often highly dynamic and far from thermal, as well as mechanical, equilibrium. In particular, for our own solar-terrestrial system, various plasma active phenomena frequently occur such as solar flares, coronal plasma heating, solar wind acceleration, and coronal mass ejections in the solar atmosphere; interplanetary magnetic clouds and collisionless shock waves in interplanetary space; and geomagnetic storms and substorms (also called Earth’s aurora) in Earth’s magnetosphere and ionosphere. Such phenomena are not only the most important events that are changing the space environment around our anthrosphere, but also provide natural laboratories for us to study in detail basic plasma processes encountered in astrophysics.

Record 171 of 193

Convective Cell Generation by Kinetic Alfven Wave Turbulence in the Auroral Ionosphere

Zhao, J. S.; Wu, D. J.; Yu, M. Y.; Lu, J. Y.

PHYSICS OF PLASMAS

卷: 19; 期: 6; 页: 062901-1-062901-5

Modulation of convective cells by kinetic Alfven wave (KAW) turbulence is investigated. The interaction is governed by a nonlinear dispersion relation for the convective cells. It is shown that KAW turbulence is disrupted by excitation of the large-scale convective motion through a resonant instability. Application of the results to the auroral ionosphere shows that cross-scale coupling of the KAW turbulence and convective cells plays an important role in the evolution of ionospheric plasma turbulence.

Record 172 of 193

Kinetic Alfven Wave Instability Driven By Field-Aligned Currents in Solar Coronal Loops

Chen, L.; Wu, D. J.


卷: 754; 期: 2; 页: 123-129

Magneto-plasma loops, which trace closed solar magnetic field lines, are the primary structural elements of the solar corona. Kinetic Alfven wave (KAW) can play an important role in inhomogeneous heating of these magnetoplasma structures in the corona. By the use of a low-frequency kinetic dispersion equation, which is presented in this paper and is valid in a finite-beta plasma with Q < beta < 1 plasma (where beta is the kinetic to magnetic pressure ratio and Q = m(e)/m(i) is the mass ratio of electrons to ions), KAW instability driven by a field-aligned current in the current-carrying loops in the solar corona is investigated. The results show that the KAW instability can occur in wave number regimes 0 < k(z) < k(z)(c) and 0 < k(perpendicular to) < k(perpendicular to)(c), and that the critical wave numbers k(z)(c) and k(perpendicular to)(c) and the growth rate both considerably increase as the drift velocity V-D of the current-carrying electrons increases in the loops. In particular, for typical parameters of the current-carrying loops in the solar corona this instability mechanism results in a high growth rate of KAWs, omega(i) similar to 0.01-0.1 omega(ci) similar to 10(3)-10(4) s(-1). The results are of importance in understanding the physics of the electric current dissipation and plasma heating of the current-carrying loops in the solar corona.

Record 173 of 193


67

Dispersion Equation of Low-Frequency Waves Driven by Temperature Anisotropy

Chen, L.; Wu, D. J.

Plasma Science and Technology

卷: 14; 期: 10; 页: 880-885

The plasma temperature (or the kinetic pressure) anisotropy is an intrinsic characteristic of a collisionless magnetized plasma. In this paper, based on the two-fluid model, a dispersion equation of

low-frequency (ω ωci, ωci the ion gyrofrequency) waves, including the plasma temperature anisotropy effect, is presented. We investigate the properties of low-frequency waves when the parallel temperature exceeds the perpendicular temperature, and especially their dependence on the propagation angle, pressure anisotropy, and energy closures. The results show that both the instable Alfvén and slow modes are purely growing. The growth rate of the Alfvén wave is not affected by the propagation angle or energy closures, while that of the slow wave depends sensitively on the propagation angle and energy closures as well as pressure anisotropy. The fast wave is always stable. We also show how to elaborate the symbolic calculation of the dispersion equation performed using Mathematica Notebook.

Record 174 of 193

Resonant Wave-Particle Interactions Modified By Intrinsic Alfvenic Turbulence

Wu, C. S.; Wang, C. B.; Wu, D. J.; Lee, K. H.

PHYSICS OF PLASMAS

卷: 19; 期: 8; 页: 082902-1-082902-5

The concept of wave-particle interactions via resonance is well discussed in plasma physics. This paper shows that intrinsic Alfven waves can qualitatively modify the physics discussed in conventional linear plasma kinetic theories. It turns out that preexisting Alfven waves can affect particle motion along the ambient magnetic field and, moreover, the ensuing force field is periodic in time. As a result, the meaning of the usual Landau and cyclotron resonance conditions becomes questionable. It turns out that this effect leads us to find a new electromagnetic instability. In such a process intrinsic Alfven waves not only modify the unperturbed distribution function but also result in a different type of cyclotron resonance which is affected by the level of turbulence. This instability might enable us to better our understanding of the observed radio emission processes in the solar atmosphere.

Record 175 of 193

Water Content, Chlorine and Hydrogen Isotope Compositions of Lunar Apatite.

Wang, Y.; Guan, Y.; Hsu, W.; Eiler, J. M.

METEORITICS & PLANETARY SCIENCE

卷: 47; 页: A397

The Moon has been thought to have a bulk planetary water content < 1 ppb [1]. Recent ion microprobe analyses have shown that lunar samples contain up to 7000±1000 ppm OH

- (reported as equivalent H2O) in

apatite and 4-46 ppm in igneous glass [2-6]. These studies suggest that the mantle sources of at least some lunar magmas contain from 64 ppb to 200 ppm [4-6]. Sharp et al. [6] report an apparently contradictory observation – that

37Cl values of lunar samples vary

from -1 to 24‰, with an upper extreme they argue demands devolatilization of anhydrous melts. We examine this issue further through measurements of water content, δ

37 Cl, and δD of apatite from lunar

meteorites MIL 05035, NWA 2977, and Dhofar 458.

Record 176 of 193

Petrology and Mineralogy of the Tissint Olivine-Phyric Shergottite

Hsu, Weibiao; Wu, Yunhua; Jiang, Yun


卷: 47; 页: A197-A197

Tissint is a recent fall of Martian meteorites on July 18, 2011. It is a geochemically depleted olivine-phyric shergottite [1]. Here we report its petrology and mineralogy.

Record 177 of 193

Oxygen Isotopes of Al-Rich Chondrules from Unequilibrated Ordinary Chondrites

Hsu, W.; Guan, Y.; Jiang, Y.; Wang, Y.


卷: 47; 页: A196-A196

Al-rich chondrules (ARCs) are a rare constituent of chondrites. They have relatively high bulk Al2O3 content (> 10 wt %), which is due to the presence of Al-rich phases, such as plagioclase, spinel, Al-rich glass etc. [1]. ARCs share some chemical and petrologic characteristics with Ca, Al-rich inclusions (CAIs), and may represent a genetic link between ferromagnesian chondrules and CAIs.

Laboratory for Astrochemistry and

Planetary Sciences


68

Twelve ARCs were found in unequilibrated ordinary chondrites (UOCs) GRV 022410 (H4), GRV 052722 (H3.7), GRV 020104 (H3.4), GRV 050016 (H3.7), GRV 050009 (H3.6), and Julesburg (L3.6) [2]. They contain bulk

Al2O3 ～ 16-33 wt% and exhibit igneous textures

comprised of olivine, diopside, plagioclase, spinel, and glass…

Record 178 of 193

Petrogenesis of the Northwest Africa 4734 basaltic lunar meteorite

Wang, Ying; Hsu, Weibiao; Guan, Yunbin; Li, Xianhua; Li, Qiuli; Liu, Yu; Tang, Guoqiang

GEOCHIMICA ET COSMOCHIMICA ACTA

卷: 92; 页: 329-344

We report the petrography, mineralogy, trace element abundance geochemistry, and Pb-Pb geochronology of the lunar meteorite Northwest Africa (NWA) 4734 and make a comparison with the LaPaz Icefield (LAP) 02205/02224 low-Ti lunar basaltic meteorites. NWA 4734 is an unbrecciated low-Ti mare basalt composed mainly of subophitic-textured pyroxene (60 vol%) and plagioclase (30%). Pyroxene, plagioclase, and olivine exhibit large compositional variations and intra-grain chemical zoning. Pyroxene and plagioclase in NWA 4734 have rare earth element (REE) concentrations and patterns similar to those of the LAPs. The crystallization age of NWA 4734, determined in situ in baddeleyite, is 3073 +/- 15 Ma (2 sigma), nearly identical to that of the LAPs (3039 +/- 12 Ma). NWA 4734 and the LAPs have similar textures, modal abundances, mineral chemistry, and crystallization ages, and are most likely source-crater paired on the Moon.One baddeleyite grain in LAP 02224 displays distinctively older and spatially variable ages, from 3349 +/- 62 to 3611 +/- 62 Ma (2 sigma), similar to another baddeleyite grain (3109 +/- 29 to 3547 +/- 21 Ma) reported by Zhang et al. (2010) for the same meteorite. Raman spectra, cathodoluminescence, and stoichiometric studies of the baddeleyite suggest that the two older grains were not endogenic but were trapped by the parental magma. Equilibrium partition calculation shows that the parental melt from which the NWA 4734 plagioclase crystallized has much lower REE contents than its whole rock, indicating an open system during magma evolution. NWA 4734 could have originated from a parental melt with REE concentrations similar to that of the Apollo 12 olivine basalt. The magma likely assimilated a small amount (similar to 4 wt%) of KREEP-rich material during its ascent through the lunar crust.

Record 179 of 193

Petrogenesis of Grove Mountains 020090: An Enriched "Lherzolitic" Shergottite

Jiang, Yun; Hsu, Weibiao


卷: 47; 期: 9; 页: 1419-1435

Grove Mountains (GRV) 020090 is a lherzolitic shergottite found in the Grove Mountains, Antarctica. It exhibits two distinct textures: poikilitic and nonpoikilitic. In poikilitic areas, large pyroxene oikocrysts enclose subhedral olivine and chromite chadacrysts. Pyroxene oikocrysts are zoned from pigeonite cores to augite rims. In nonpoikilitic areas, olivine, pyroxene, and interstitial maskelynite occur as major phases, and minor phases include chromite and merrillite. Compared with typical lherzolitic shergottites, GRV 020090 contains a distinctly higher abundance of maskelynite (19 vol%). Olivine and pyroxene are more ferroan (Fa2840, En5772Fs2431Wo414 and En4653Fs1721Wo2635), and maskelynite is more alkali-rich (Ab4365Or27). The major phases, whole-rock (estimated) and fusion crust of GRV 020090, are relatively enriched in light rare earth elements (LREE), similar to those of the geochemically enriched basaltic shergottites, but distinct from those of LREE-depleted lherzolitic shergottites. Combined with a high oxygen fugacity of log fO2 = QFM - 1.41 +/- 0.04 (relative to the quartz-fayalite-magnetite buffer), it is clear that GRV 020090 sampled from an oxidized and enriched mantle reservoir similar to those of other enriched shergottites. The calculated REE abundances and patterns of the melts in equilibrium with the cores of major phases are parallel to but higher than that of the whole rock, suggesting that GRV 020090 originated from a single parent magma and experienced progressive fractional crystallization in a closed system. The crystallization age recorded by baddeleyite is 192 +/- 10 (2s) Ma, consistent with the young internal isochron ages of enriched shergottites. Baddeleyite dating results further demonstrated that the young ages, rather than ancient ages (>4 Ga), appear to represent the crystallization of Martian surface lava flow. GRV 020090 shares many similarities with Roberts Massif (RBT) 04261/2, the first enriched lherzolitic shergottite. Detailed comparisons suggest that these two rocks are petrologically and geochemically closely related, and probably launch paired.

Record 180 of 193

Distribution of PSF of Near Earth Object Survey Telescope

Li, Bin; Zhao, Haibin


卷: 53; 期: 3; 页: 240-248

The field of view of CCD in NEOST(Near Earth Object Survey Telescope)is 1.94°*1.94°.As a wide-field

Xuyi Observation Station


69

telescope,the focusing according to single stars leads to uneven distribution of PSF(Point Spread Function)due to the field curvature.The contour map of PSFs FWHM(Full Width at Half Maximum)indicates the features of the distribution of PSF.The focal surface is yielded by fitting the relation between defocus and PSFs FWHM. It is confirmed that the focal surface reshaped by the field lens is not flat but convex,and the distance from the peak to the valley is about(855)mum.The center of the distribution of PSF deviates from the CCD center.This phenomenon is considered to be caused by the inclination of CCD.The method of getting the best-focus can be found by using the histogram of PSFs FWHM.

Record 181 of 193

The 2009 Apparition of Methuselah Comet 107P/Wilson-Harrington: A Case of Comet Rejuvenation?

I. Ferrín; Hiromi Hamanowa; Hiroko Hamanowa; J. Hernández; E. Sira; A. Sánchez; Zhao, H.; R. Miles

PLANETARY AND SPACE SCIENCE

卷: 70; 期: 1; 页: 59-72

The 2009 apparition of comet 107P was observed with a variety of instruments from six observatories. The main results of this investigation are: (1) 107P/Wilson-Harrington was found to be active not only in 1949 but also in 1979, 1992, 2005 and 2009. The activity is very weak and produces only a slight brightness increase above the nucleus. (A(SEC)=V-NUC(1,1,0)-m(1,1) < 1 mag). Since the amount of solar energy received by the object at perihelion has been monotonically increasing since 1928, we conclude that the comet has been active at all apparitions ever after. The probability that the activity in 1949 or in 2009 was due to a surface impact is very small. (2) The rotational period has been determined. We find P-ROT=6.093 +/- 0.002 h. The amplitude of the rotational light curve (peak to valley) is A(ROT) = 0.20 +/- 0.01 mag in V. From this data the minimum ratio of semi-axis is (a/b)(MIN) = 1.20 +/- 0.02. The rotational light curve is identical to the shape of a saw tooth. The shape of the object must be peculiar and has sharp edges. (3) This is the first time that the phase curve of a comet has been determined in three colors, B, V and R. We find B(1,1,alpha)= 16.88( +/- 0.06)+ 0.041( +/- 0.001)alpha, V(1,1,alpha)=16.31(+/- 0.04) + 0.043( +/- 0.001)alpha, and R(1,1,alpha) = 15.90( +/- 0.04) + 0.039( +/- 0.001)alpha. (4) From the phase curves color indices can be deduced when the comet is not active. We find V-B=0.57 +/- 0.07 and V-R=0.41 +/- 0.06. (5) Assuming a geometric albedo p(v)=0.04 and the absolute magnitude from the phase plot, we find an effective diameter free from rotational modulation D-EFFE = 3.67 +/- 0.06 km. (6) The secular light curves are presented. The comet is slightly active above the nucleus line (A(SEC)(1,LAG)= 0.36 +/- 0.10 mag), but did not exhibited a coma. Activity started +26 +/- 1 d after

perihelion. Using the definition of photometric age, we find T-AGE = 4700 (+6000, - 1700) cy (comet years), an exceedingly old object, a methuselah comet. (7) In the 2009 apparition no tail and no coma were detected using more sensitive detectors than on 1949. This is good evidence to conclude that this object is very near extinction and belongs to the graveyard of comets. In a Remaining Revolutions vs. Water-Budget Age plot, we have identified the region of the graveyard, and 107P is a member of this group. (8) Using the amplitude of the secular light curve (A(SEC)) vs. Diameter (D-EFFE) diagram (Fig. 15), we show that 107P is the most evolved object in the current data base of comets. In the classification scheme of Ferrin (PSS, 58, 365-391, 2010), 107P is a methuselah comet (WB-AGE = 7800 > 100 comet years), medium size (1A < D-EFFE = 3.67 < 6 km) nucleus, fast rotating (P-ROT = 6.093 h < 7 h). belonging to the graveyard of comets (the region with A(SEC) < 1 mag in Fig. 15 or 1.000 cy < WB-AGE in Fig. 18), that must be very near its dormant phase, were not for the fact that this comet is temporarily being rejuvenated due to a trend of apparitions with decreasing perihelion distances. (9) Since the general flow of the sample is down and to the left in the A(SEC) vs.D-EFFE diagram, and since this flow has been going on for centuries, and since dwarf comets evolve much more rapidly than large comets, the existence of a significant population of dormant and extinct comets located in the lower left region of the diagram is predicted This is the graveyard Three comets have been identified as members of the graveyard, 107P, 133P and D/1891W1 Blanpain.

Record 182 of 193

The ASTROD I Charging Simulation and Disturbances Due To Solar Energetic Particles at 0.5 AU

Bao, Gang

ACTA ASTRONAUTICA

卷: 77; 页: 29-33

The electrostatic charging of ASTROD I test mass (the Astrodynamical Space Test of Relativity using Optical Devices I) will disturb its pure geodesic motion due to spurious Coulomb and Lorentz forces. The three main disturbances associated with the charging are the acceleration noise of the test mass, the coupling between the test mass and the spacecraft, the appearance of unwanted coherent Fourier components in the measurement bandwidth. By implementing the same geometry and physics models in our previous work, a positive charging rate of 9369 e(+)/s for the solar energetic particles (SEPs) event on October 19th

Laboratory for Planetary Science and

Deep Space Exploration


70

1989 is predicted. Based on these charging rates, we calculated the acceleration noise and stiffness associated with charging. We also compared the acceleration noises arising from Coulomb and Lorentz effects using different discharge characteristics. Although the noise due to charging exceeds the ASTROD I budget for the two events at 0.5 AU, it can be suppressed through continuous discharging. In addition to Monte Carlo uncertainty, an error of +/- 30% in the net charging rates was added to account for uncertainties in the primaries spectra, physics and geometry models.

Record 183 of 193

Predicting the Configuration of a Planetary System: KOI-152 Observed By Kepler

Wang, Su; Ji, Jianghui; Zhou, Ji-Lin


卷: 753; 期: 2; 页: 170-179

The recent Kepler discovery of KOI-152 reveals a system of three hot super-Earth candidates that are in or near a 4:2:1 mean motion resonance. It is unlikely that they formed in situ; the planets probably underwent orbital migration during the formation and evolution process. The small semimajor axes of the three planets suggest that migration stopped at the inner edge of the primordial gas disk. In this paper, we focus on the influence of migration halting mechanisms, including migration "dead zones," and inner truncation by the stellar magnetic field. We show that the stellar accretion rate, stellar magnetic field, and the speed of migration in the protoplanetary disk are the main factors affecting the final configuration of KOI-152. Our simulations suggest that three planets may be around a star with low star accretion rate or with high magnetic field. On the other hand, slow type I migration, which decreases to one-tenth of the linear analysis results, favors forming the configuration of KOI-152. Under such a formation scenario, the planets in the system are not massive enough to open gaps in the gas disk. The upper limits of the planetary masses are estimated to be about 15, 19, and 24M(circle plus), respectively. Our results are also indicative of the near Laplacian configurations that are quite common in planetary systems.

Record 184 of 193

Tidal Evolution of Exo-Planetary Systems: WASP-50, GJ 1214 and CoRoT-7

Dong, Yao; Ji, JiangHui


卷: 55; 期: 5; 页: 872-979

We perform numerical simulations to investigate tidal evolution of two single-planet systems, that is, WASP-50 and GJ 1214 and a two-planet system CoRoT-7.

The results of orbital evolution show that tidal decay and circularization may play a significant role in shaping their final orbits, which is related to the initial orbital data in the simulations. For GJ 1214 system, different cases of initial eccentricity are also considered as only an upper limit of its eccentricity (0.27) is shown, and the outcome suggests a possible maximum initial eccentricity (0.4) in the adopted dynamical model. Moreover, additional runs with alternative values of dissipation factor Q'(1) are carried out to explore tidal evolution for GJ 1214b, and these results further indicate that the real Q'(1) of GJ 1214b may be much larger than its typical value, which may reasonably suggest that GJ 1214b bears a present-day larger eccentricity, undergoing tidal circularization at a slow rate. For the CoRoT-7 system, tidal forces make two planets migrating towards their host star as well as producing tidal circularization, and in this process tidal effects and mutual gravitational interactions are coupled with each other. Various scenarios of the initial eccentricity of the outer planet have also been done to investigate final planetary configuration. Tidal decay arising from stellar tides may still work for each system as the eccentricity decreases to zero, and this is in association with the remaining lifetime of each planet used to predict its future.

Record 185 of 193

The Simulation of Radiation Effects to Astronauts Due To Solar Energetic Particles in Deep Space

Bao, Gang

ACTA ASTRONAUTICA

卷: 71; 期: 5; 页: 32-37

The exposure to interplanetary radiation poses a serious health risk to astronauts, especially for long-term missions. Protecting the astronauts from these particles has been the key issue to the manned space mission. High-energy space particles can penetrate the protective layer of a spacecraft, and probably cause deleterious effects to the astronauts. To estimate the size of these effects, a credible simulation of radioprotection is required. Using the Geant4 software toolkit, we have modeled the interaction processes and predicted the total energy deposit in a phantom (astronaut) as well as the similar information associated with secondary effects, due to Solar Energetic Particles (SEPs) at similar to 1 AU caused by the large SEPs events in October 1989 and August 1972. In addition, we compared the characteristics of the energy deposit due to SEPs and Galactic Cosmic Rays (GCRs) and explained the differences between them by physical mechanism analysis.

Record 186 of 193

The Internal Structure Models of Europa

Jin, Sheng; Ji, JiangHui


71

ACTA ASTRONAUTICA

卷: 55; 期: 1; 页: 156-161

We model the interior of Europa using a method by which we set three layers of Europa and the composition of each layer in advance. Comparing the calculated mass and radius related to each model with the data derived by the observations, we propose three possible internal structure models for Europa. All models are assumed to be differentiated into a metallic core, a (Mg, Fe)(2)SiO4 silicate mantle and an outer water shell. The only difference amongst these models are the composition of the core. The core of Model I is composed of Fe, while Model II composed of FeS, and the two models are based on the inferences provided by Europa's external gravitational field. Model III has a core which consists of Fe-FeS alloy, similar to that of Earth's outer core. Model I has a Fe core with a radius of 431 km, a (Mg,Fe)(2)SiO4 mantle with 999 km and a water shell with 132 km. Model II has a 777 km FeS core, a 619 km (Mg,Fe)(2)SiO4 mantle and a 167 km water shell. Model III has a 571 km Fe-0.8(FeS)(0.2) core, a 832 km (Mg,Fe)(2)SiO4 mantle and a 166 km water shell. In all three models, the density range and the radius of each layer is consistent with those deduced by Anderson et al.

Record 187 of 193

Possible Origin of the Damocloids: The Scattered Disk or a New Region?

Wang, Su; Zhao, Hai-Bin; Ji, Jiang-Hui; Jin, Sheng; Xia, Yan; Lu, Hao; Wang, Min; Yao, Jin-Sheng


卷: 12; 期: 11; 页: 1576-1584

The Damocloids are a group of unusual asteroids that recently added a new member: 2010 EJ104. The dynamical evolution of the Damocloids may reveal a connection from the Main Belt to the Kuiper Belt and beyond the scattered disk. According to our simulations, two regions may be considered as possible origins of the Damocloids: the scattered disk, or a part of the Oort cloud, which will be perturbed to a transient region located between 700 AU and 1000 AU. Based on their potential origin, the Damocloids can be classified into

two types, depending on their semi-major axes, and about 65.5% of the Damocloids are classified into type I which mainly originate from the Oort cloud. Whether the Damocloids are inactive nuclei of the Halley Family of Comets may depend on their origin.

Record 188 of 193

Grain Growth in Protoplanetary Disks

Lu, Tao; Ji, Jianghui


卷: 30; 期: 3; 页: 284-301

In star-formation theory, a flat, rotating disk always formed after star formation in the molecular cores which own initial angular momentum. It is so-called protoplanetary disk, which consists of gas and dust. The mass ratio of gas to dust is 100: 1. Gas may be accreted onto the central star, or dissipated through photoevaporation, radiation pressure and in/outflow. Portion of dust is dissipated or accreted because it is coupled strongly with gas, and others will further grow from interstellar dust (sub-mum) to planetesimal (10 km) or planet finally. Dust growth can be confirmed by observation features, e.g., statistical investigations of presence of dust emission as a function of age, Si-O stretching vibrations in silicates around 10 mum and the analysis of the size and optical depth structure of silhouette disks. In growth process, the key issue is collision adhesion. There are various mechanisms that lead to collision, so collision velocities may distribute in a broad range. However, dust growth is not synchronized. The timescales of growth differ in the various locations in the disk. At the same time, the exchange of material still occurs in the disk for inflow/outflow, sedimentation, etc. Hence, the collision process will be quite complex and the outcomes may be diverse. These results dominate the growth process of dust. In this sense, dust growth may directly have influence on the properties of protoplanetary disk and planetary formation. Therefore, the study can not only improve the understanding of characteristics of a protoplanetary disk, but also reveal the scenario of material evolution at the early stage of planetary formation, by investigating the process of dust growth in the protoplanetary disk.

V. Joint Institute for Particle Nuclear Physics & Cosmology

Record 189 of 193

On Dark Energy Models of Single Scalar Field

Li, Mingzhe; Qiu, Taotao; Cai, Yifu; Zhang, Xinmin


卷: 2012; 期: 04; 页: 003

In this paper we revisit the dynamical dark energy model building based on single scalar field involving

higher derivative terms. By imposing a degenerate condition on the higher derivatives in curved spacetime, one can select the models which are free from the ghost mode and the equation of state is able to cross the cosmological constant boundary smoothly, dynamically violate the null energy condition. Generally the Lagrangian of this type of dark energy models depends on the second derivatives linearly. It behaves like an imperfect fluid, thus its cosmological perturbation theory needs to be generalized. We also


72

study such a model with explicit form of degenerate Lagrangian and show that its equation of state may cross - 1 without any instability.

Record 190 of 193

Search for Dark Matter Signals with Fermi-LAT Observation of Globular Clusters NGC 6388 and M15

Feng, Lei; Yuan, Qiang; Yin, Peng-Fei; Bi, Xiao-Jun; Li, Mingzhe


卷: 2012; 期: 04; 页: 030

The globular clusters are probably good targets for dark matter (DM) searches in gamma-rays due to the possible adiabatic contraction of DM by baryons. In this work we analyse the three-year data collected by Fermi Large Area Telescope of globular clusters NGC 6388 and M 15 to search for possible DM signals. For NGC 6388 the detection of gamma-ray emission was reported by Fermi collaboration, which is consistent with the emission of a population of millisecond pulsars. The spectral shape of NGC 6388 is also shown to be consistent with a DM contribution if assuming the annihilation final state is b (b) over bar. No significant gamma-ray emission from M 15 is observed. We give the upper limits of DM contribution to gamma-ray emission in both NGC 6388 and M 15, for annihilation final states b (b) over bar, W+W-, mu(+)mu(-), tau(+)tau(-) and monochromatic line. The constraints are stronger than that derived from observation of

dwarf galaxies by Fermi.

Record 191 of 193

Metric-Affine Formalism of Higher Derivative Scalar Fields in Cosmology

Li, Mingzhe; Wang, Xiulian


卷: 2012; 期: 07; 页: 010

Higher derivative scalar field theories have received considerable attention for the potentially explanations of the initial state of the universe or the current cosmic acceleration which they might offer. They have also attracted many interests in the phenomenological studies of infrared modifications of gravity. These theories are mostly studied by the metric variational approach in which only the metric is the fundamental field to account for the gravitation. In this paper we study the higher derivative scalar fields with the metric-affine formalism where the affine connection is treated arbitrarily at the beginning. Because the higher derivative scalar fields couple to the connection directly in a covariant theory these two formalisms will lead to different results. These differences are suppressed by the powers of the Planck mass and are usually expected to have small effects. But in some cases they may cause non-negligible deviations. We show by a higher derivative dark energy model that the two formalisms lead to significantly different pictures of the future universe.


73

VI. Other

Record 192 of 193

A Study on the Celestial Phenomena and Chronology Recorded in the Ancient Text and the Modern Text of the Bamboo Annals

Zhang Jian; Zhang Peiyu


卷: 53; 期: 2; 页: 126-136

The Bamboo Annals is the history book unearthed by West Jin Dynasty in the tomb of Wei King of the third century BC,It recorded a lot of chronology and historical facts of the Xia Shang Zhou period,but the Bamboo Annals gradually lost during 12 or 13 century.Today there are two sorts of the Bamboo Annals we can read,one is the Ancient Text of the Bamboo Annals compiled by the modern scholars,the other is an entire book called the Modern Text of the Bamboo Annals.The latter was probably found by Yuan or Ming Dynasty.The Modern Text of the Bamboo Annals is different from the Ancient Text on the writing and contents,more of celestial phenomena are recorded to the Modern Text of the Bamboo Annals than to the Ancient Text.It is discussed in this paper that the celestial phenomena and chronology are recorded in the Bamboo Annals,the results show that these celestial phenomena of the Modern Text of the Bamboo Annals are not original records unearthed by West Jin Dynasty in the tomb of Wei King of the third century BC, but were supplemented by the scholars of Song and Yuan

Dynasties.

Record 193 of 193

A Study on Marss Stay at Twenty-eight Lunar Mansions, Four-planet Conjunctions and Five-planet Conjunctions during Past Dynasties of China

Zhang Jian


卷: 53; 期: 4; 页: 299-307

There are a lot of records about planets motions during past dynasties of China in Tian Wen Zhi.The Marss stay at twenty-eight lunar mansions,four-planet conjunctions and five-planet conjunctions are studied in this paper with the calculational methods of modern astronomy and Shou-shi Calendar.The results show that there are a lot of mistakes in these records.The proportion of mistakes is 51%in 65 records of Marss stay at twenty-eight lunar mansions,50%in 12 records of four-planet conjunctions,and 18%in 11 records of five-planet conjunctions.The main causes of mistakes are also discussed in this paper and they are as follows:(1) There is no unified format of date for the Mars stay at twenty-eight lunar mansions;(2) There is no unified format of the time duration for the Mars stay at twenty-eight mansions;(3) There are mistakes in the recorded patterns of Mars motions;(4) There are also mistakes in the records of four-planet conjunctions and five-planet conjunctions;(5) Mistakes were made in editing and publishing.


74

紫台历年发表论文情况

专著

1. Inclination Function in Satellite Dynamics.

吴连大, 汪宏波, 马静远. 科学出版社, ISBN:

978-7-0303-5857-8

2. Kinetic Alfvén Wave: Theory, Experiment,

and Application. 吴德金 . 科学出版社 ,

ISBN: 978-7-0303-6124-0

获奖

1. 国家自然科学奖二等奖，“高能电子宇宙射线

能谱超出 ” 的发现，常进 , 证书号：

2012-Z-102-2-04-R01

2. 国家科技进步特等奖,“嫦娥二号工程”，常

进，单位排名 25，个人排名 40，证书号：

2012-J24201-0-01-R40

3. 中国科学院优秀导师奖，史生才

4. 中国科学院王宽诚人才奖，中国科学院王宽诚

博士后工作奖励基金，王争

5. 中国科学院院长特别奖，任远

6. 中国科学院院长优秀奖，晋升

7. 中国科学院朱李月华奖，孙荣煜

8. 江苏省教育科技系统五一巾帼标兵岗称号，近

地天体探测和太阳系天体研究团组，马月华

Annual Report’2012

75

专利

序号类型名称发明人专利号状态

1 发明专利毫米波、亚毫米波段集成型外差式阵列

接收机

单文磊,

杨戟 201210355636.9 申请

2 发明专利大口径透射式望远镜系统张晓祥 201210471996.5 申请

3 发明专利天文望远镜多通道定时装置许占伟,

王歆 201210270557.8 申请

4 发明专利以固态半导体源谐波为参考源的量子

级联激光器锁相系统

缪巍,张

文 201210081557.3 申请

5 发明专利阵列成像系统张文,缪

巍 201210028016.4 申请

6 发明专利宽带和高分辨率毫米波亚毫米波信号

检测系统

史生才,

林镇辉 CN200710130929.6 授权

7 发明专利宽带和高分辨率毫米波亚毫米波信号

检测方法

史生才,

林镇辉 CN200710130930.9 授权

8 发明专利多像元超导探测器接收系统及太赫兹

信号检测方法

史生才,

林镇辉 CN201010560189.1 授权

9 发明专利波导型边带分离超导隧道结混频器基

座单文磊 CN201010509654.9 授权

10 发明专利毫米波多像元制冷接收机杜瓦单文磊 CN201010509975.9 授权

11 发明专利一种基于图像全帧扫描的空间碎片检

测方法

张晓祥,

鲁春林 CN201010160062.0 授权

12 发明专利一种全帧 CCD 图像处理方法平一鼎,

张晓祥 CN201010187659.4 授权

13 发明专利一种空间碎片的检测系统张晓祥,

鲁春林 CN201010160212.8 授权


76

2012 年度发表科研论文、专著、专利一览表

团组与学科片论文

总数

第一

单位

论文

SCI

论文

第一单

位 SCI

论文

国际

合作

论文

专

著

专利

申请

专利

授权

宇宙学、暗物质及高能天体物理研究 4 2 3 1 0 0 0 0

宇宙伽玛暴、中子星及相关物理研究 8 6 5 4 4 0 0 0

太阳高能及相关物理过程研究 22 12 13 6 8 0 0 0

太阳活动的多波段观测研究 8 8 5 5 1 0 0 0

暗物质和空间天文实验室 16 9 11 4 6 0 0 0

暗物质和空间天文 58 37 37 20 19 0 0 0

恒星结构、演化和脉动研究 1 0 1 0 1 0 0 0

南极天文中心 10 1 8 1 5 0 0 0

星系宇宙学和暗能量研究 1 1 1 1 0 0 0 0

星系中的恒星形成研究 15 6 13 4 9 0 0 0

分子云与恒星形成研究 17 3 17 3 16 0 0 0

毫米波和亚毫米波技术实验室 24 12 11 1 10 0 3 5

青海观测站 8 5 4 1 5 0 0 0

南极天文和射电天文 76 28 55 11 47 0 3 5

空间目标与碎片观测研究中心 17 17 5 5 0 1 2 3

卫星精密定轨及应用研究 2 2 0 0 0 0 0 0

CCD 相机研制实验室 3 3 0 0 0 0 0 0

应用天体力学和空间目标与碎片 22 22 5 5 0 1 2 3

近地天体探测和太阳系天体研究 3 1 3 1 2 0 0 0

历算和天文参考系研究 3 3 2 2 0 0 0 0

太阳和太阳系等离子体研究 12 10 11 9 3 1 0 0

天体化学和行星科学实验室 5 5 5 5 3 0 0 0

盱眙天文观测站 2 1 1 0 1 0 0 0

行星科学和深空探测实验室（筹） 7 7 6 6 0 0 0 0

行星科学和深空探测 32 27 28 23 9 1 0 0

管理和支撑 2 2 0 0 0 0 0 0

其他汇总 5 0 5 0 0 0 0 0

总计 193 116 128 59 76 2 5 8


77

紫台主要科研项目统计

学术报告

序

号日期报告人单位职称题目

1 2012/1/20 Henrik Beuther Max-Plank Institute for

Astronomy 博士

High-mass star formation:

From galactic structures to

the initial conditions

2 2012/1/16 苏萌哈佛大学博士

The Discovery of Giant

Gamma-ray Bubbles in the

Milky Way

3 2012/2/10 HuiDong

National Optical

Astronomy

Observatory

博士

Multi-band HST mapping

of dusty clouds in the

nuclear bulge of M31

4 2012/2/10 Sophia DAI CfA/Harvard SEDs of dust rich quasars

at z < 3 '

5 2012/2/13 Rainer Spurzem

National Astronomical

bservatoriesof China,

Chinese Academy of

Sciences

GPU Supercomputing in

China and Application to

supermassiveblack holes

and gravitational waves

from galactic nuclei

6 2012/2/14 Randall Smith High Energy

Astrophysics Division 博士

In-Progress and Future

X-ray Satellite Missions


78

序


Smithsonian

Astrophysical

Observatory

7 2012/3/20 Dana Longcope

Department of Physics

at Montana State

University

教授

Slow shocks and

conduction fronts from

Petschek reconnection of

skewed magnetic fields:

two-fluid effects

8 2012/3/31 尔欣中国家天文台博士

Constraint of halo

properties using weak

lensing flexion

9 2012/5/10 李荐扬

Department of

Astronomy University

of Maryland at College

Park

博士 Dawn at Vesta: A Whole

New World

10 2012/4/17 Jean-Claude Vial 法国空间天体物理研究

所（IAS）教授

Some new results from

solar space observations

11 2012/4/24 李菂

国家天文台射电研究部

首席科学家，FAST 项目

科学家，“射电天文前沿

及 FAST 早期科

学”(973)首席科学家

研究

员

Building a Paradigm of

Star Formation

12 2012/4/25 Gregory Herczeg KIAA/PKU 教授 Herschel's view of

low-mass star formation

13 2012/5/4 Wang Haimin New Jersey Institute of

Technology 教授

Back reaction of solar

flares

14 2012/5/15 Chunhua Qi

Harvard-Smithsonian

Center for

Astrophysics

博士 Molecular observations of

protoplanetary disks

15 2012/6/1 Daniela Calzetti 教授

Star Formation Scaling

Laws: What Works and

What Does Not?

16 2012/6/22 Paolo D'Avanzo

INAF-Osservatorio

Astronomico di Brera,

Italy

博士

Dynamical studies of

Accreting Millisecond

X-ray Pulsars

17 2012/6/22 Andrew Gould Ohio State University

Microlensing Planets: A

controlled Scientific

Experiment Drawn From


79

序


Absolute Chaos

18 2012/7/9 Han Xianming 美国 Butler 大学博士 Asteroid rotation studies

19 2012/7/19 Wei Cui Purdue University 教授 Rapid Gamma Ray Flaring

of Active Galactic Nuclei

20 2012/8/29 Sera Markoff University of

Amsterdam 教授

David vs. Goliath:

exploiting the black hole

mass scale to constrain jet

physics

21 2012/8/1 Chang-Mo Ryu

Department of

Physics, POSTECH,

Pohang, South Korea

Nonlinear relativistic

Weibel instability

22 2012/8/20 Yuriy Voitenko

Space Physics Division,

Belgian Institute for

Space Aeronomy,

B-1180 Brussels,

Belgium

教授

Kinetic Alfven

Turbulencein Space

Plasmas

23 2012/8/19 Thijs de Graauw

director of the joint

ALMA observatory

(Chile)

教授

The Atacama Large

Millimeter/submillimeter

Array (ALMA):

Construction and Early

Science

24 2012/8/9 Andrea Melandri

(INAF-Osservatorio

Astronomico di Brera,

Italy

Hunting for progenitors:

the GRB-Supernova

connection

25 2012/8/16 Lyndsay Fletcher University of Glasgow

Flare heating and particle

acceleration in the solar

chromosphere

26 2012/8/13 王新国家天文台扩散激波加速机制的蒙特卡

洛模拟

27 2012/8/16 Hugh Hudson UC Berkeley 研究

员

Solar flares observed in

white light and in the EUV

28 2012/8/17 王然亚利桑那大学

Studying Quasar-host

Galaxy Evolution at

Redshift 6 with Large

Millimeter and Radio

Interferometer Arrays

29 2012/8/17 吕南姚加州理工学院


80

序


30 2012/8/7 吴娟中国地质大学<武汉> PAMELA 宇宙线粒子的测量

及宇宙线传播模型的研究

31 2012/9/3 Yang Liu (刘扬） Stanford University

(斯坦福大学) 博士

Magnetic helicity in

emerging active regions

computed from the HMI

data

32 2012/8/31 Padelis P.

Papadopoulos 德国马普射电天文所博士

CO Lines as H2 Mass

Estimators, Energy Source

and SF Mode Indicators

33 2012/9/3 Martin Bureau 牛津大学，名古屋大学

Molecular gas and star

formation in early-type

galaxies

34 2012/9/3 Rosie Chen 德国马普射电天文所

Resolved

Schmidt-Kennicutt

Relation on Star Forming

Regions in the Galaxy and

Magellanic Clouds

35 2012/9/4 Martin Bureau 牛津大学，名古屋大学

The Tully-Fisher Relation:

Across Morphological

Types and Redshifts

36 2012/9/3 宿英娜

Harvard-Smithsonian

Center for

Astrophysics

Observations and

Magnetic Field Modeling

of the Solar Flare/CME

Event on 2010 April 8

37 2012/9/4 陆埮中科院紫金山天文台院士《百年宇宙学》

38 2012/9/20 Alain Omont IAP

Herschel high-z

submillimeter galaxies and

gravitational lenses. H2O,

a new diagnosis of their

dense cores

39 2012/9/25 Xundong Sun 斯坦福大学博士

Magnetic Field and Energy

Evolution in a Major Active

Region Observed by

SDO/HMI

40 2012/9/29 SHEN Renfeng 澳大利亚多伦多大学博士

"The Evolution of

Accretion Disk in Tidal

Disruption Events"

41 2012/10/26 Warrick Andrew The University of New 教授 The nearest youngest


81

序


Lawson South Wales stellar associations

42 2012/10/26 Cheuk-Yu Edward

TONG

Harvard-Smithsonian

Center for

Astrophysics

博士

Instruments at the Front

Lines of Submillimeter

Astronomy: The

Submillimeter Array and

Greenland Telescope?

Status and Plans?

43 2012/10/29 Li, Zhiyuan (UCLA) 博士

Feeding and feedback of

super-massive black holes:

inflows and outflows in the

two nearest galactic nuclei

44 2012/11/9 刘超国家天文台副研 The mixed origins of the

Milky Way thick disk

45 2012/11/20 A. Struminsky (IKI, Moscow)

Dynamics of temperature

and emission measure of

solar flare plasma

46 2012/11/20 L.I.

Miroshnichenko (IZMIRAN, Moscow)

（a）Solar Cosmic Rays: 70

Years of Ground-Based

Observations; (b)

Radiation Hazard in Space:

Extreme Fluxes in Solar

Energetic Particle Events.

47 2012/11/22 L.I.

Miroshnichenko (IZMIRAN, Moscow)

（a）Solar Cosmic Rays: 70

Years of Ground-Based

Observations; (b)

Radiation Hazard in Space:

Extreme Fluxes in Solar

Energetic Particle Events.

48 2012/11/20 Ir. T.M. Klapwijk

Delft University of

Technology, the

Netherlands

教授

Superconductors for

multipixel detectors at

submm wave lenghts

49 2012/11/28 崔晓红国家天文台伽玛暴的前身星及暴周环境

50 2012/11/27 郭琦国家天文台星系形成

51 2012/12/6 毛业伟中国科学技术大学博士

Effects of Stellar

Population and Dust

Attenuation on UV and IR

Observational Properties

of Galaxies


82

序


52 2012/12/13 Lucas Uhm KIAA/ UNLV

Dynamics and Afterglows

of GRB Blast Waves with a

Long-lived Reverse Shock

53 2012/12/17 盘军国家天文台研究

员宇宙大尺度结构的统计分析

54 2012/12/25 舒新文中国科学技术大学博士

Census of high-redshift

star-forming galaxies in

cluster fields

55 2012/12/29 Shori Torii 日本早稻田大学

CALET 首席科学家教授 CALET on space station


83

国际合作与台内学术报告统计

团组与学科片出访

人次占比

来访

人次占比

台内学

术报告占比

宇宙学、暗物质及高能天体物理研究 2 1% 0 0% 1 2%

宇宙伽玛暴、中子星及相关物理研究 0 0% 3 2% 2 4%

太阳高能及相关物理过程研究 12 8% 30 20% 11 20%

太阳活动的多波段观测研究 5 3% 7 5% 2 4%

暗物质和空间天文实验室 25 17% 19 13% 7 13%

暗物质和空间天文研究部汇总 44 29% 59 39% 24 44%

恒星结构、演化和脉动研究 0 0% 0 0% 0 0%

南极天文中心 7 5% 7 5% 4 7%

星系宇宙学和暗能量研究 2 1% 15 10% 2 4%

星系中的恒星形成研究 17 11% 14 9% 15 28%

分子云与恒星形成研究 20 13% 18 12% 3 6%

毫米波和亚毫米波技术实验室 29 19% 30 20% 3 6%

青海观测站 7 5% 0 0% 0 0%

南极天文和射电天文研究部汇总 82 54% 84 55% 27 50%

空间目标与碎片观测研究中心 6 4% 0 0% 0 0%

卫星精密定轨及应用研究 0 0% 0 0% 0 0%

CCD 相机研制实验室 0 0% 0 0% 0 0%

应用天体力学和空间目标与碎片汇总 8 5% 0 0% 0 0%

近地天体探测和太阳系天体研究 1 1% 0 0% 0 0%

历算和天文参考系研究 8 5% 2 1% 1 2%

太阳和太阳系等离子体研究 3 2% 5 3% 1 2%

天体化学和行星科学实验室 0 0% 0 0% 0 0%

盱眙天文观测站 5 3% 1 1% 1 2%

行星科学和深空探测实验室（筹） 2 1% 1 1% 1 2%

行星科学和深空探测研究部汇总 19 13% 9 6% 4 7%

总计 151 100% 152 100% 54 100%


84

中国 2012 年度“十大天文科技进展”

（紫金山天文台相关部分）

1、嫦娥二号伽玛谱仪探测研究取得新进展

嫦娥二号伽玛谱仪观测数据表明，月球表面东

海与危海盆地在其形成时，撞击深度应该到达了下

月壳，撞击事件可能把月球深层次的物质挖掘了出

来。该研究利用嫦娥二号伽玛谱仪对月球表面大型

撞击坑及其周围溅射物放射性元素含量的观测，提

出了上述观点。文章将发表在 4 月 8 号 Nature

Scientific Reports 上。

在嫦娥二号工程中，中国科学院紫金山天文台

暗物质和空间天文实验室承担伽玛谱仪的研制与数

据分析工作。与嫦娥一号相比，嫦娥二号伽玛谱仪

在世界上首次采用先进的溴化澜(LaBr3)闪烁晶体

作为主探测器，碘化铯(CsI)作为反符合晶体成功抑

制空间及卫星本底。嫦娥二号伽玛谱仪的灵敏度远

高于世界同类探测器,能敏感的区分月球表面元素

的细微差别,为后期的数据分析及科学研究提供了

坚实的基础。

目前国际上对于东海和危海盆地形成时的撞

击深度存在较大的争议。以危海盆地为例，早期的

研究认为危海撞击事件仅仅到达了上月壳。但最近

日本学者通过分析”月亮女神 Kaguya”的光谱数

据在该盆地边缘发现了富含橄榄石的区域，推测危

海撞击事件可能击穿月壳，把月幔的物质挖掘了出

来。嫦娥二号伽玛谱仪新的探测结果证实危海盆地

周围物质富含放射性元素，但丰度较低。这说明，

危海盆地在形成时撞击事件穿透 KREEP 岩层的可

能性较小。根据月球岩浆洋最新模型及这两个区域

钾元素丰度的分析，研究推测危海撞击事件可能仅

仅撞击到月壳侵入的岩层。

图 1：钾元素在东海、危海区域的分布图


2、太赫兹量子级联激光器技术研究取得突破进展

太赫兹及远红外波段高分辨率光谱观测对于理

解近邻宇宙物质循环主要物理过程、恒星与星际介

质间物质循环等有重要作用。受限于太赫兹波段参

考信号源技术，该频段高灵敏度、高频谱分辨率接

收机仍然亟待发展。近年来，一种新型太赫兹固态

信号源量子级联激光器（QCL）取得了飞速发展，

但自由振荡 QCL 激光器难以满足天文观测应用。针

对太赫兹 QCL 激光器锁相这一前沿研究方向，中国

科学院紫金山天文台毫米波与亚毫米波技术实验室

与荷兰 SRON/TUDelft、美国 MIT 等团队开展了

合作研究。利用更先进的三阶分布反馈式量子级联

激光器及高灵敏度太赫兹超导热电子混频器，首次

实现了基于太赫兹 QCL 激光器的频率可调外差式

混频接收机。在此基础上，又利用太赫兹气体吸收

谱线成功实现了对太赫兹 QCL 激光器的频

率锁定，并同时实现了功率稳定，从而在国际上首

次实现了基于频率与功率同时稳定 QCL 激光器的

太赫兹外差混频接收机（参见图 2）。这一研究成果

将应用于建议中的 NASA 太赫兹望远镜计划

GUSSTO，也有望应用于我国的南极太赫兹望远镜

计划和载人空间站工程太赫兹应用项目。

紫金山天文台任远博士作为第一作者完成的相

关研究论文发表于 Appl. Phys. Lett. 97 (2010),

161105; 98 (2011), 231109; 100 (2012),

041111; 101 (2012), 101111，并在该领域重要国

际会议 11th Int. Conf. Intersubband Transitions

in Quantum Wells 上作特邀报告，也因此获 2012

年中科院院长特别奖。

图 2 3.5THz 三阶 DFB QCL 激光器（左）、超导 HEB 热电子混频器（中）和太赫兹 QCL 锁相前后中频检测信号对比（右）

3、精确确定图塔蒂斯轨道嫦娥二号拓展试验任务取得重大应用成果

继圆满完成探月先导技术验证既定任务和飞

赴日地 L2 点试验任务之后，嫦娥二号卫星于 2012

年 12 月 13 日 16:30，在距地球约 700 万千米远的

深空，精确实现与 4179 号小行星图塔蒂斯的近距

离飞越探测，在国际上第一次成功获取了小行星的

高分辨率光学图像（见图 3），成像距离为 93 km，

交会距离为 3.2 km，相对速度为 10.73 km/s。这

是我国首次实现对小行星的深空探测，也是国际上

首次实现对图塔蒂斯的近距离探测。

精确确定图塔蒂斯轨道成为嫦娥二号拓展任

务能否成功的关键。在探月与航天工程中心精心部

署、院月球与深空探测总体部统一安排下，中国科

学院利用国内兴隆、盱眙、丽江观测站，以及夏威

夷大学、智利 CTIO 天文台等 5 个台站的 6 台光学

天文望远镜，对图塔蒂斯进行观测，自 2012 年 5

月至 11 月，共获得有效观测数据 300 余组，所有

观测数据全部汇合到我们团队进行分析处理。中科

院紫金山天文台季江徽研究员率领的团队利用观测

数据连续对图塔蒂斯小行星进行了轨道确定，定轨

内符合精度优于 5 km，这个结论一致通过专家评

审，定轨结果为卫星系统所采用并直接应用在拓展

任务中，为嫦娥二号近距离飞越图塔蒂斯小行星提

供了重要的科学依据和工程保障。


86

为满足工程任务需求，该团队对图塔蒂斯的测

定轨精度进行了详细地分析、对飞越时刻拍照策略

及预期小行星成像效果进行模拟仿真，结果可信，

在获得光学图像后也得到了很好地验证。此外，还

紧密配合卫星总体工作，对嫦娥二号卫星在轨对月

成像结果、卫星惯性姿态和拍照策略等进行多方面

复核。

该团队精确确定了图塔蒂斯轨道，使嫦娥二号

实现了对其千米级近距离飞越探测，圆满地完成拓

展试验任务。2013 年 1 月，中科院公布的 2012

年重大科技成果指出，“我院还在国家重大科技任

务的组织实施中发挥了重要作用，承担的相关科技

任务取得重要进展。例如在载人航天与探月工程重

大科技专项中……嫦娥二号拓展试验的相关重大任

务，取得一批高水平应用研究成果。 ”

（ http://www.cas.cn/xw/zyxw/201301/t20130

121_3755067.shtml）

图 3 “嫦娥二号”再拓展试验任务中拍摄的图塔蒂斯小行星

4、首次对太阳在氦原子谱线 10830Å 进行高分辨率成像，并观测到了向上能流的超精细结构

中国科学院紫金山天文台季海生研究员和美

国同行合作，利用最新落成的大口径太阳望远镜

(大熊湖天文台1.6米口径的NST) 和我国自行研制

的 10830Å 窄带滤光器，首次得到了太阳在该波段

的高分辨率图像(色球)，发现了超精细(～100 公里)

的磁流管结构，这些结构扎根在米粒之间，被认证

为高温物质和能量外流的通道。该研究成果解释了

加热日冕的能量究竟来自光球的何处。其可能物理

过程是：光球米粒不断的对流运动，通过挤压形成

米粒间小尺度强磁场，小尺度强磁场中的活动产生

了高温物质和能量的外流。工作刊登在 2012 年 5

月份出版的《天体物理快报》上 (APJL,v750, L25)。

NASA 官网遂即就该研究成果进行了新闻发布。

太阳的外层大气具有反常的温度分布，加热日

冕到百万度高温的能量从何而来，即是著名的“太

阳日冕加热问题”，该问题被《科学》杂志列为天体

物理八大问题之一。本成果的发现有望彻底解决这

一问题。

http://www.cas.cn/xw/zyxw/201301/t20130121_3755067.shtml

http://www.cas.cn/xw/zyxw/201301/t20130121_3755067.shtml


87

图 4: (a) 作为本次成果的太阳局部的 10830Å 的像, (b) 进一步的局部像, (a)和(b)的背景为透射的光球像. 左边的三幅从上往下依次

是 8 次电离铁离子谱线 171Å、氦原子谱线 10830Å和氧化钛分子谱线 7057Å 同时和同一区域的像, 分别对应着低日冕、色球和光球. 往

上流出的 10830Å 吸收物质来自于绿色箭头所指的地方, 在吸收物质流出的同时发生了远紫外增亮。

If you are interested in the work of PMO please contact division of Science & Technology Management at

+86-(0)25-83332288, 83332018 [email protected]


research annual report 2012 · 2019. 9. 16. · zhangyin zhao, jin chan, sheng-cai shi, yuehua ma,...

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