The Evolution & Structure of Pulsar Wind Nebulae

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• Radio: Filaments – Expanding PWN encounters filaments, compress & increase n & B enhance synchrotron emission (Jun 1998, Bucciantini et al. 2004) • No X-ray: – High energy electron suffer synchrotron loss 3
Filaments • X-ray filaments <strong>of</strong> 3C58: associated with radio, not with optical different mechanism -magnetic loops torn from the toroial field by kink instabilities 3
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 10 and 11: Emission & Spectra of nebulae • T
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: • Optical: Filaments - R-T instab
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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