Multiwavelength Studies of Pulsar Wind Nebulae

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•! PWN model with evolved power !law electron spectrum fits X-ray!and TeV emission!- Fermi emission falls well above!model!HESS J1640-465!Slane et al. 2010!•! Modifying low-energy electron!spectrum by adding Maxwellian!produces GeV emission through!inverse Compton scattering!- primary contribution is from IR!from dust (similar to Vela X)!- mean energy (!"10 5 ) and fraction!in power law ("4%) consistent w/!particle acceleration models!•! GeV emission can also be fit w/!pion model!- requires n 0 > 100 cm -3 , too large!for G338.3-0.3!Patrick Slane (CfA)High-Energy Emission from Pulsars and Their SystemsSant Cugat 2010
G327.1-1.1: More (Reverse) Shocking Results!•! G327.1-1.1 is a composite SNR!for which radio morphology!suggests PWN/RS interaction!•! Chandra observations show!an offset compact source w/!trail of nonthermal emission!extending back to radio PWN!- compact source is extended !and embedded in bowshock-!structure!- prong-like structures extend!from source, inflating bubble!in region cleared out by RS!Temim et al. 2009!Patrick Slane (CfA) High-Energy Emission from Pulsars and Their Systems Sant Cugat 2010
Page 1 and 2: Multiwavelength Studies !Collaborat
Page 3 and 4: Jet/Torus and Ejecta Structure in P
Page 5 and 6: •! G54.1+0.3 is a young !PWN !- t
Page 7 and 8: Broadband Emission from PWNe!Gelfan
Page 9 and 10: Injection from Relativistic Shocks!
Page 11 and 12: Evolution in an SNR: Vela X!LaMassa
Page 13 and 14: HESS J1640-465!5 arcmin!•! Extend
Page 15 and 16: HESS J1640-465!•! Extended source
Page 17: •! PWN model with evolved power !
Page 21 and 22: Probing Composite SNRs With Fermi!
Page 23: Summary!•! Multiwavelength studie

Multiwavelength Studies of Pulsar Wind Nebulae

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