Neutron Star Environment: from Supernova Remnants to Pulsar Wind Nebulae
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Transcript of Neutron Star Environment: from Supernova Remnants to Pulsar Wind Nebulae
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HKU Fermi Workshop
Neutron Star Environment:from Supernova Remnants
to Pulsar Wind Nebulae
Stephen C.-Y. NgMcGill University
Special thanks to Pat Slane for some materials in this talk
Jun 21, 2010
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HKU Fermi Workshop
Outline SNRs and PWNe are important Galactic
Gamma-ray sources
High energy emission of SNRs Cosmic ray acceleration Gamma-ray production
Overview of PWNe PWNe in Gamma-rays
Jun 21, 2010
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HKU Fermi Workshop
Supernova Remnants
Jun 21, 2010
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Forward shock
Reverse shock
Den
sit
y
Radius
Shock Physics
Jun 21, 2010
Reverse shock
Forwardshock
ISMEjecta Contact
discontinuity
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HKU Fermi Workshop
Thermal X-ray emission
Thermal X-ray spectrum temperature (107K) and density
Radius age
Jun 21, 2010
E
Rv
n0
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HKU Fermi Workshop
Non-thermal SNRs Cosmic ray acceleration in strong shocks B-field + relativistic particles = synchrotron 274 known Galactic SNRs, < 10 synchrotron-
dominated– e.g. SN1006, Vela Jr, G347.3−0.5
Non-thermal features in historical SNRs– e.g. Cas A, Tycho
Jun 21, 2010
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HKU Fermi Workshop
Allen 2000thermal
nonthermalNon-thermal Emission
Jun 21, 2010
Allen 2000
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HKU Fermi WorkshopEnergy (keV)
Coun
ts/k
eV
Cassam-Chenai et al. 2007
SN 1006
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HKU Fermi Workshop
Tycho
Forward Shock(nonthermal electrons)
Warren et al. 2005
Reverse Shock(ejecta – Fe,K)
Jun 21, 2010
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HKU Fermi Workshop
Gamma-ray Production2cme
h
h
2cme
0
Leptonic: Inverse-Compton scattering of electrons by CMB, far IR, or star light
Hadronic: Inelastic scattering of protons by nucleons Neutral Pion decay
See talks by Thomas Tam and Bo Zhang
Jun 21, 2010
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HKU Fermi Workshop
HESS
Aharonian et al. 2006
Similar morphology in X-ray and TeV suggests I-C emissionbut spectrum seems to suggest 0 -decay
G347.3-0.5 (RX J1713.7-3946)
Acero et al. 2009
XMM
Jun 21, 2010
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Fermi Detection
Jun 21, 2010NASA/DOE/Fermi LAT Collaboration
Abdo et al. 2009
W51C
Abdo et al. 2010
W44
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Pulsar Wind Nebulae
Jun 21, 2010
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HKU Fermi Workshop
Where does the pulsar rotational energy go? E>1035erg/s < 10% in radiation (mostly Gamma-rays) > 90% in pulsar winds
http://www.astroscu.unam.mx/neutrones/NS-Picture/MagSphe/MagSphe.html
Pulsar Wind
Jun 21, 2010
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HKU Fermi Workshop
Pulsar Wind
Jun 21, 2010
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PWN within SNR
ISMShoc
ked
ISM
Shoc
ked
Ejec
ta
Unsh
ocke
d Ej
ecta
PWN
Pulsa
r Win
d
Forward ShockReverse ShockPWN Shock
PulsarTerminationShock
Gaensler & Slane (2006)
Terminationshock
c c/3
Pulsar wind Ejecta
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HKU Fermi Workshop
Bow-shocks
Jun 21, 2010
NASA/CXC/Gaensler et al.
IC 443
NASA/CXC/SAO/NF/SNRAO/VLA /Gaensler et al.
The Mouse
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HKU Fermi WorkshopNASA/CXC/Palomar/2MASS/NRAO
Broadband Emission
Jun 21, 2010
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Axisymmetric Structure
Jun 21, 2010
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HKU Fermi Workshop
Torus+jet
Jun 21, 2010
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HKU Fermi Workshop
Time Variability
NASA/ASU/J.Hester et al
Jun 21, 2010
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HKU Fermi Workshop
Gamma-ray Emission
synchrotron
Abdo et al. (2010)
Jun 21, 2010
Crab PWN
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HKU Fermi Workshop
TeV PWNe Vela X
LaMassa et al. (2008)Aharonian et al. (2006)
NASA/PSU/G.Pavlov et al.
Jun 21, 2010
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HKU Fermi WorkshopAbdo et al. (2010)
Vela X
de Jager et al. (2008)
Jun 21, 2010
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HKU Fermi Workshop
G0.9+0.1
LaRosa et al. (2000) Aharonian et al. (2005)
Jun 21, 2010
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HKU Fermi Workshop
MSH 15-52 / PSR B1509-58
Aharonian et al. (2005) NASA/CXC/SAO/P.Slane et al.
Jun 21, 2010
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HKU Fermi Workshop
Kookaburra Complex
Aharonian et al. (2006)
Jun 21, 2010
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HKU Fermi Workshop
Aharonian et al. (2006)
PSR B1823-13
XMMG18.0-0.7
Jun 21, 2010
Gaensler et al. 2003
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HKU Fermi Workshop
Summary SNRs and PWNe are important Galactic
Gamma-ray source
Broadband emission from radio to TeV
Hadronic and Leptonic scenarios of Gamma-ray production
Fermi can fill up the gap between X-ray and TeV in the SED
Jun 21, 2010