neutron star environment: from supernova remnants to pulsar wind nebulae stephen c.-y. ng mcgill...
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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
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
HKU Fermi Workshop
Supernova Remnants
Jun 21, 2010
Forward shock
Reverse shock
Den
sit
y
Radius
Shock Physics
Jun 21, 2010
Reverse shock
Forwardshock
ISMEjecta Contact
discontinuity
HKU Fermi Workshop
Thermal X-ray emission
Thermal X-ray spectrum temperature (107K) and density
Radius age
Jun 21, 2010
E
R
v
n0
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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
HKU Fermi Workshop
Allen 2000
thermal
nonthermal
Non-thermal Emission
Jun 21, 2010
Allen 2000
HKU Fermi WorkshopEnergy (keV)
Counts
/keV
Cassam-Chenai et al. 2007
SN 1006
HKU Fermi Workshop
Tycho
Forward Shock(nonthermal electrons)
Warren et al. 2005
Reverse Shock(ejecta – Fe,K)
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Gamma-ray Production
2cme
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
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
Fermi Detection
Jun 21, 2010
NASA/DOE/Fermi LAT Collaboration
Abdo et al. 2009
W51C
Abdo et al. 2010
W44
Pulsar Wind Nebulae
Jun 21, 2010
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
HKU Fermi Workshop
Pulsar Wind
Jun 21, 2010
PWN within SNR
ISM
Sh
ock
ed ISM
Sh
ock
ed E
ject
a
Unsh
ock
ed
Eje
cta
PW
N
Puls
ar
Win
d
Forward Shock
Reverse ShockPWN Shock
PulsarTerminationShock
Gaensler & Slane (2006)
Terminationshock
c c/3
Pulsar wind Ejecta
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
HKU Fermi Workshop
NASA/CXC/Palomar/2MASS/NRAO
Broadband Emission
Jun 21, 2010
Axisymmetric Structure
Jun 21, 2010
HKU Fermi Workshop
Torus+jet
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Time Variability
NASA/ASU/J.Hester et al
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HKU Fermi Workshop
Gamma-ray Emission
synchrotron
Abdo et al. (2010)
Jun 21, 2010
Crab PWN
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TeV PWNe
Vela X
LaMassa et al. (2008)Aharonian et al. (2006)
NASA/PSU/G.Pavlov et al.
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Abdo et al. (2010)
Vela X
de Jager et al. (2008)
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G0.9+0.1
LaRosa et al. (2000) Aharonian et al. (2005)
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MSH 15-52 / PSR B1509-58
Aharonian et al. (2005) NASA/CXC/SAO/P.Slane et al.
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HKU Fermi Workshop
Kookaburra Complex
Aharonian et al. (2006)
Jun 21, 2010
HKU Fermi Workshop
Aharonian et al. (2006)
PSR B1823-13
XMMG18.0-0.7
Jun 21, 2010
Gaensler et al. 2003
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