Observations of Bow-Shock Pulsar Wind Nebulae - Chandra X-Ray ...

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• Note that in pre-Sedov! phase, sound speed is! lower in reverse shock! region than in outer! SNR! Cruising at the Reverse Shock! Patrick Slane (CfA)! SNRs and PWNe in the Chandra Era! Boston 2009!
Summary! I. Observations of Bow Shock PWNe! #- High-resolution studies reveal similar underlying ! structure to static PWNe! - Morphology provides measure of Mach number! - Knowledge of surroundings provides Ė, pulsar velocity! - Questions remain on detailed structure of innermost regions! II. Transition Objects! - As pulsars approach supersonic speeds, PWN morphology is distorted! toward bow shock geometry! - More modeling required to study the structure in this stage ! III. Bow Shocks Near the Reverse Shock! - At least some fast pulsars should form bow-shock-like structures! well inside SNRs, as they pass through the reverse shock! - This has impact for interpretation of pulsar velocities, and! possibly as a probe of ejecta! Patrick Slane (CfA)! SNRs and PWNe in the Chandra Era! Boston 2009!
Page 1 and 2: Observations of! Pulsar Bowshock Ne
Page 3 and 4: Bow Shock PWNe: Introduction! • F
Page 5 and 6: Gaensler et al. 2004! Bow Shock PWN
Page 7 and 8: • If pulsar is moving through SNR
Page 9 and 10: Olbert et al. 2001! Bow Shock PWNe
Page 11 and 12: PWNe in Transition? G327.1-1.1! Pat
Page 13: • Note that in pre-Sedov! phase,

Observations of Bow-Shock Pulsar Wind Nebulae - Chandra X-Ray ...

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