snr rxj1713.7-3946 kev/tev联合观测, 轻子?强子?
DESCRIPTION
Best observations in TeV----shell-type SNRs give us more know about CRs acceleration----diffusive shock acceleration But electron or hadron?. SNR RXJ1713.7-3946 keV/TeV联合观测, 轻子?强子?. A&A. 449 (2006) 223-242. A&A , 464(2007)235-243. 距离: 1 kpc 年龄: 1600 年 半径: 1 度 流强( 1TeV ): 70%Crab. - PowerPoint PPT PresentationTRANSCRIPT
![Page 1: SNR RXJ1713.7-3946 keV/TeV联合观测, 轻子?强子?](https://reader036.vdocuments.mx/reader036/viewer/2022082206/56813c90550346895da63a78/html5/thumbnails/1.jpg)
Best observations in TeV----shell-type SNRsgive us more know about CRs acceleration----diffusive shock accelerationBut electron or hadron?
![Page 2: SNR RXJ1713.7-3946 keV/TeV联合观测, 轻子?强子?](https://reader036.vdocuments.mx/reader036/viewer/2022082206/56813c90550346895da63a78/html5/thumbnails/2.jpg)
SNR RXJ1713.7-3946 keV/TeV联合观测,轻子?强子?
A&A , 464(2007)235-243
轻子模型
强子模型
A&A. 449 (2006) 223-242
距离: 1 kpc
年龄: 1600 年
半径: 1 度
流强( 1TeV ):70%Crab
![Page 3: SNR RXJ1713.7-3946 keV/TeV联合观测, 轻子?强子?](https://reader036.vdocuments.mx/reader036/viewer/2022082206/56813c90550346895da63a78/html5/thumbnails/3.jpg)
SNR RXJ1713.7-3946 keV/TeV联合观测, +GeV观测,偏向于强子?
A&A , 464(2007)235-243
轻子模型
强子模型
A&A. 449 (2006) 223-242
Fermi 初步结果
距离: 1 kpc
年龄: 1600 年
半径: 1 度
流强( 1TeV ):70%Crab
![Page 4: SNR RXJ1713.7-3946 keV/TeV联合观测, 轻子?强子?](https://reader036.vdocuments.mx/reader036/viewer/2022082206/56813c90550346895da63a78/html5/thumbnails/4.jpg)
![Page 5: SNR RXJ1713.7-3946 keV/TeV联合观测, 轻子?强子?](https://reader036.vdocuments.mx/reader036/viewer/2022082206/56813c90550346895da63a78/html5/thumbnails/5.jpg)
New anisotropy component and corotation evidence of the GCR (Science 314(2006)439-443)
New anisotropy componentAmp=0.16% w/o corotation;Observation: 0.03%±0.03%.
Celestial Intensity map (E~3TeV)
Intensity @ E~300TeV
![Page 6: SNR RXJ1713.7-3946 keV/TeV联合观测, 轻子?强子?](https://reader036.vdocuments.mx/reader036/viewer/2022082206/56813c90550346895da63a78/html5/thumbnails/6.jpg)
6
All-particle spectrum measured by Tibet-III array(ApJ 678, 1165-1179 (2008))
A sharp knee around 4 PeV is clearly seen.
Jing Huang (ISVH2008-PARIS)
Model Knee Position
(PeV)
Index of spectrum
QGS.+HD
4.0± 0.1 R1= -2.67± 0.01
R2= -3.10± 0.01
QGS.+PD
3.8± 0.1 R1= -2.65± 0.01
R2= -3.08± 0.01
SIB.+HD 4.0± 0.1 R1= -2.67± 0.01
R2= -3.12± 0.01
![Page 7: SNR RXJ1713.7-3946 keV/TeV联合观测, 轻子?强子?](https://reader036.vdocuments.mx/reader036/viewer/2022082206/56813c90550346895da63a78/html5/thumbnails/7.jpg)
Diffuse Gamma Rays from Galactic Plane
0°60°120°180° 180°240°300°-10°
10°
0°
EGRET data
Electronmodel Electron
model
0 model0 model
![Page 8: SNR RXJ1713.7-3946 keV/TeV联合观测, 轻子?强子?](https://reader036.vdocuments.mx/reader036/viewer/2022082206/56813c90550346895da63a78/html5/thumbnails/8.jpg)
已有的多波段观测 +100TeV γ射线观测有助于确定宇宙线强子源A&A , 464(2007)235-243
强子模型
距离: 1 kpc
年龄: 1600 年
半径: 1 度
流强( 1TeV ):70%Crab
SNR RXJ1713.7-3946100TeVγ射线的观测极大地增强了我们对宇宙线强子源的认识,
![Page 9: SNR RXJ1713.7-3946 keV/TeV联合观测, 轻子?强子?](https://reader036.vdocuments.mx/reader036/viewer/2022082206/56813c90550346895da63a78/html5/thumbnails/9.jpg)
Background and signal
![Page 10: SNR RXJ1713.7-3946 keV/TeV联合观测, 轻子?强子?](https://reader036.vdocuments.mx/reader036/viewer/2022082206/56813c90550346895da63a78/html5/thumbnails/10.jpg)
![Page 11: SNR RXJ1713.7-3946 keV/TeV联合观测, 轻子?强子?](https://reader036.vdocuments.mx/reader036/viewer/2022082206/56813c90550346895da63a78/html5/thumbnails/11.jpg)
宇宙线的成份和能谱
LHC的千万倍!
超出
主要是原子核: P , He ,… , Fe,…
也有:, e±
还有: γ , ν
最高宇宙线粒子的能量达到3×1020eV,约 50焦耳。从那里,又是如何被加速到这样的能量还是一个未解的迷
宇宙线电子,伽玛射线,中微子对宇宙线起源,加速,对暗物质寻找,对量子引力研究有重要意义。