The Evolution & Structure of Pulsar Wind Nebulae

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Emission & Spectra of nebulae • The nature of this spectral steepening is not understood; theory above is based on a simple pow-law assumption. • Rapid decline of injection (inherent spectrum deviate from power-law?), modifications from discrete acceleration sites, all contribute to a complicated integrated spectrum. • “As a result, the interpretation of spectral steepening as being due to synchrotron losses can lead to drastically wrong conclusions about PWN properties.” 1
Observationally • Detailed structrues: Crab especially • 40-50 PWN • Category: – Composite (with a shell-like SNR) – Crab-like – Cometary (pulsar with high v, few) • Evolution 1
Page 1 and 2: The Evolution & Structure of 2007-0
Page 3 and 4: • SNR => pulsar-driven SNR => PWN
Page 5 and 6: Theoretically Theoreticall • Marv
Page 7 and 8: Pulsar Wind-magnetodynamic Wind mag
Page 13 and 14: Evolution • Phase I - Expanding i
Page 15 and 16: Phase I 1
Page 20: Torus, Jet, Wisp & Filament 2
Page 24: • G54.1+0.3: luminosity, geometry
Page 27 and 28: Wisp ACIS-S3 (11/3/2000- 4/6/2001)
Page 29 and 30: • Optical: Filaments - R-T instab
Page 31 and 32: Filaments • X-ray filaments of 3C
Page 33 and 34: Phase II Phase III 3
Page 35 and 36: Phase II Phase III 3
Page 37 and 38: Phase III Phase IV 3
Page 39: Other & Recent results • Very you

The Evolution & Structure of Pulsar Wind Nebulae

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