rapporteur talk: acceleration and propagation of cr ...igor v. moskalenko 31 rapporteur talk “many...
TRANSCRIPT
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RapporteurRapporteur talk:talk:
Acceleration and Propagation of CRAcceleration and Propagation of CR
Sections OG 1.3, OG 1.4, HE 1.2 (theory)Sections OG 1.3, OG 1.4, HE 1.2 (theory)
Igor V. MoskalenkoIgor V. Moskalenko
NASA Goddard Space Flight CenterNASA Goddard Space Flight [email protected]
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Igor V. Moskalenko 2 Rapporteur talk
Covered Topics
TeV electrons
10Be and other radioactive secondariesLight stable secondaries (d,3He,LiBeB)
New effects in CR propagation
LiBeB production cross sectionsAntiprotons, anti- d,t,3He,4He
Propagation models/codes
OG1.3OG1.3
Shocks in SNRShocks in the Galactic wind
Shocks in the galaxy clusters
Relativistic shocks/jets,pair plasma
OG1.4OG1.4
Knee: DiffusionMore in the rapporteur
talk by Prof. TakitaKnee: Sources
HE1.2HE1.2
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Igor V. Moskalenko 3 Rapporteur talk
CR Interactions in the Interstellar Medium
e+-
Sources:SNRs, Shocks,Superbubbles
Particle accelerationPhoton emission P
HeCNO
X,γ
gas
gas
B
ISRF
π
e+-
+-
P_
LiBeB
ISM
diffusionenergy losses
reaccelerationconvection
etc. π0
synchrotron
IC
bremss
Chandra
GLAST
ACE
BESS
Halo
disk
escape
PHe
CNOsolar
modulation
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Igor V. Moskalenko 4 Rapporteur talk
Fixing Propagation Parameters: Standard Way
Using secondary/primary nuclei ratio:•Diffusion coefficient and its index•Propagation mode and its parameters (e.g., reacceleration VA, convection Vz)
Radiactive isotopes:Galactic halo size Zh
Zh increase
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Igor V. Moskalenko 5 Rapporteur talk
Radioactive Secondaries @ 1 GeV/nucleon
Two reasons for the discrepancy
with ISOMAX data
20 mb
Uncertainties in the production cross sectionUncertainties in the production cross section
Energy Zh, halo size
Energy Zh, halo size
NO wind
Convection(Voelk)
The energy dependence the halo sizeThe energy dependence the halo size
Non-trivial energy dependence of the diffusion coefficient
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Igor V. Moskalenko 6 Rapporteur talk
Effect of Local Environment
Sun
~200pc
Local Bubble:
A hole in the interstellar gas is formed in a series of SN explosions; some shocks may still exist there…
May be important for radioactive CR species, but Dxx(local)≠Dxx(average)?
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Igor V. Moskalenko 7 Rapporteur talk
Radioactive Secondaries: Effect of the LB
Two-zones diffusion model includes the “local hole”.
The effect on radioactive secondaries:
10Be (2.17 Myr) 36Cl (0.443 Myr)
Data “prefer” Rhole>0: B/C, 10Be/9Be, 36Cl/Cl
26Al (1.31 Myr)26Al/27Al – difficulty:Errors in CS or astrophysical data Anisotropy problem ?
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Igor V. Moskalenko 8 Rapporteur talk
Radioactive Secondaries: Effect of the LB
Weighted slab calculations:
Local Bubble affects radioactive secondaries
26Al/27Al
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Igor V. Moskalenko 9 Rapporteur talk
Stable Secondaries: 3He, LiBeB
Study of propagation of light secondaries using GALPROP model.
Problem: Reacceleration model gives too few antiprotons in CR
Test:“Standard” reacceleration model vs. reacceleration model with LB component
He/Si=100 (GCRS)vs. 220 (LBS)
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Igor V. Moskalenko 10 Rapporteur talk
Deuterium in CR
Simplified models:• Leaky-Box• Convection• Reacceleration
The uncertainties:• Cross sections• Modulation for He & d
ΦΦ=500 MV=500 MV
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Igor V. Moskalenko 11 Rapporteur talk
Effect of Local Environment
Regular Galactic magnetic fieldmay establish preferentialdirections of CR propagation
Sun
GC
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Igor V. Moskalenko 12 Rapporteur talk
Collecting Regions
Regular magnetic field in the Galaxy affects the diffusion:
The importance of sources depends on their position relatively to the magnetic field line.ZM
ean
traj
ecto
ry,
kpc
Mean trajectory length for CR is a function of Z: different grammage fordifferent species (compare with leaky-box)
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Igor V. Moskalenko 13 Rapporteur talk
Production Cross Sections of LiBeB
Semi-empirical systematics are not always correct.
Results obtained by different groups are often inconsistent and hard to test.
Very limited number of nuclear measurements:
Evaluating the cross section is very laborious and can’t be done without modern nuclear codes.
Use LANL nuclear database and modern computer codes.
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Igor V. Moskalenko 14 Rapporteur talk
Antimatter: Secondary Antiprotons in CR
Uncertainties in the models:•Propagation models and parameters
Gas distribution in the GalaxyAmbient spectrum of CR (solar
modulation, GeV excess in γ’s !)Current knowledge of CR diffusion
•Production cross sections of isotopes and pbars
Typical errors 20%Fitting to B/C ratio may introduce
errors in Dxx, Dpp•Heliospheric modulation
Depends on rigiditySimilar for all nuclei A/Z~ +2Different for protons A/Z=+1 and
pbars A/Z=-1•Systematic errors of measurements
Difficult to account for
OR Astrophysical Reasons:• Change in propagation mode at LE
E.g., propagation of LE particles aligned to magnetic field lines
• Local environment (e.g. Local Bubble)Fresh “unprocessed” nuclei component at LE
• Sources of LE protons (<20 GeV)Required by diffuse gamma rays and pbars
• Population of hard-nucleon-spectrum sources with matter nearbyRequired by diffuse gamma rays and pbars
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Igor V. Moskalenko 15 Rapporteur talk
Antimatter: Light Secondary Anti-Nuclei in CR
Predictions for CR fluxes of secondary anti- d, t, 3,4He, using the coalescence model for production of the anti-nuclei and leaky-box and diffusion propagation models.
Anti-4He provides the smallest background for DM signal, but…-The signal (also coalescence) is weak-Annihilation cs is large @ LE-Heliospheric modulation
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Igor V. Moskalenko 16 Rapporteur talk
Effect of IS Turbulence on CR Transport
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Igor V. Moskalenko 17 Rapporteur talk
Effect of Local SourcesEffect of Local Sources
SNR are believed to be the sources of CR because of strong shocks waves and suitable energetics
protons/8 GeV
electrons/16 GeV
Modeling stochastic SNR events:
Protons – relatively small fluctuations
electrons/1 TeV
Electrons – large fluctuations, increase with energy
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Igor V. Moskalenko 18 Rapporteur talk
CR Fluctuations
Fluctuations of 1-1000 TeV protons and effect of close SNRs on CR anisotropy in reacceleration model and plain diffusion.
SNRs included: SN 185, RX J1713-3946, S 147, Cygnus Loop, Vela, G65.3+5.7, HB21
Excluded: RX J0852-4622 too young, inclusion will give 100 times larger anisotropy.
Reacceleration model with close SNRs is better.
Effect ofVela & S 147
reacc.Standardanisotropy
plain diff.
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Igor V. Moskalenko 19 Rapporteur talk
TeV Electrons
“GZK effect” for electrons:Sharp cutoff in the primary
electron spectrum above 100 TeV(30 TeV ?).
VHE electron measurements is a direct test of SNR origin of CR, but also a test of our local environment
100 TeV
10 TeV
1 TeV
Dist,kpcAge
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Igor V. Moskalenko 20 Rapporteur talk
Structure in the VHE Electron Spectrum
Some nearby SNRs should exhibit unique identifiable features in the electron spectrum in the range 1-10 TeV.
The most promising sources are Vela, Cygnus Loop, and Monogem.
Estimates of IC gamma-ray flux from these sources would be interesting
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Igor V. Moskalenko 21 Rapporteur talk
Models: Exponential Galaxy Model
Primary spectra:
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Igor V. Moskalenko 22 Rapporteur talk
Models: Exponential Galaxy Model
LiBeB/CNO10Be/9Be
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Igor V. Moskalenko 23 Rapporteur talk
Models: Development of a New Propagation Code
Try to solve a plain diffusion equation by the method of series expansion:Bessel functions in R, andtrigonometrical functions in φ
Reduce the 3D equation to the time dependent1-D propagation:
But, no distinctive results yet
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Igor V. Moskalenko 24 Rapporteur talk
Models: GALPROP: Web-Based Interface
Simple forms on the Web to obtain (tables & plots):Spectra of any isotope or Spectra of any isotope or element Zelement Z≤≤28 or any 28 or any combination (can choose units combination (can choose units and scale)and scale)Arbitrary isotopic ratios vs. Arbitrary isotopic ratios vs. energyenergyIsotopic distributions for any ZIsotopic distributions for any ZElemental or isotopic Elemental or isotopic abundances @ arbitrary energyabundances @ arbitrary energyAntiprotonsAntiprotonsElectrons & positronsElectrons & positrons
Modulated & interstellar Modulated & interstellar –– first first only for the solar vicinity and only for the solar vicinity and later for the whole Galaxy.later for the whole Galaxy.
http://lhea.gsfc.nasa.gov/~imos/galprop.html
Not ready yet, but check back this fall !
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Igor V. Moskalenko 25 Rapporteur talk
OG1.4: Acceleration of CR
Shocks:• SNRs• Galactic wind• Galaxy clusters
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Igor V. Moskalenko 26 Rapporteur talk
OG1.4: Acceleration of Electrons & Protons in SNR
Young SNR:• Proton index -2• Two populations of
electrons: in the “accelerator” and in the “storage”
Storage – maincontributor to IC.
Needs a strong & turbulent magnetic field toconfine relativistic electrons
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Igor V. Moskalenko 27 Rapporteur talk
Shocks in the Galactic wind: E>1015 eV
Acceleration byshocks at50-100 kpcfrom the plane
~Zx1017 eV
Low efficiency, but Myrs of time…
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Igor V. Moskalenko 28 Rapporteur talk
Particle Acceleration in the Clusters of Galaxies
Shocks associated with mergers of clusters
GLAST will be able to detect ~50 clusters
Only 10% of total diffuseemission (10 times lowerthan Loeb-Waxmanestimate for strong shocks)
Mergers: Mach number <2
10% of diffuseemission
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Igor V. Moskalenko 29 Rapporteur talk
Electrons in the Galaxy Clusters
N-body + hydrodynamicsimulations:• Shock acceleration due
to mergers• Scattering on Alfven
waves (necessary !)
Wave power spectrum ismodified presumably dueto particle acceleration
Radio emission from Coma cluster
Blasi: Alfven waves may be not very effective as energy goes to protons
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Igor V. Moskalenko 30 Rapporteur talk
HE1.2: Knee - Theory
Main reasons of the steepening:• Diffusion (2 papers, one idea –to increase the diffusion perpendicular to the plane)
• Source properties
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Igor V. Moskalenko 31 Rapporteur talk
“Many Knees” - Diffusion
• Phenomenological model “poly-gonato” reproduces the CR spectrum around the knee.
• Agrees well with simplified diffusion model which includes Hall diffusion.
Problems: •All sources @ 4 kpc - to obtain the sharp knee•No disintegration of nuclei•Importance of the structure of the regular magnetic field
Conclusion: the origin of the knee is diffusion
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Igor V. Moskalenko 32 Rapporteur talk
Diffusion Perpendicular to the Plane
• D is too small• Consider open
magnetic lines to the plane (filaments)D ~D‼
Require the Galactic wind ~500 km/s near the plane (check vs. LE CR)
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Igor V. Moskalenko 33 Rapporteur talk
Young SNRs and Bell-Lucek Mechanism
Young SNRs: • Bell-Lucek mechanism to
increase the turbulent magnetic field ahead of the shock front (AlfvenM~1000)
• Bohm diffusion• Modifications to Sedov-
Taylor solution
Acceleration up toE ≤ few 1017 eV,steeper spectrum
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Igor V. Moskalenko 34 Rapporteur talk
Superposition of Different SNR Types
SN Ia + SN II + SN Ib/c + SN IIn
Superposition of SNRs of different types: SN Ia, SN II, SN Ib/c, SN IIn
Different SN rate, power, composition
Knee ~ hypernovae
Predictions for composition
Composition
Historical variations of CR intensity should be essentialHistorical variations of CR intensity should be essential
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Igor V. Moskalenko 35 Rapporteur talk
Pulsar Origin of the Knee
Knee structure – a single SNR source, but no gamma rays.
May be pulsar: Geminga or Vela
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Igor V. Moskalenko 36 Rapporteur talk
Conclusions
Thanks to the authors of the reported papers for the education of the rapporteur in the corresponding topics.
Acknowledgments to the LOC for the beautiful organization of the conference.