Pulsar Wind Nebulae and Particle Acceleration in the Pulsar Magnetosphere

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dc.creatorShibata, S.
dc.creatorTomatsuri, M.
dc.creatorShimanuki, M.
dc.creatorSaito, K.
dc.creatorNakamura, Y.
dc.creatorMori, K.
dc.date2002-07-20
dc.date.accessioned2026-07-07T02:04:24Z
dc.date.available2026-07-07T02:04:24Z
dc.descriptionThis paper deals with the Crab Nebula problem to suggest that particle acceleration takes place not only at the inner shock but also over a larger region in the nebula with disordered magnetic field. Kennel and Cornoniti (1984) constructed a spherically symmetric model of the Crab Nebula and concluded that the pulsar wind which excites the nebular is kinetic-energy dominant (KED) because the nebula flow induced by KED wind is favorable to explain the nebula spectrum and expansion speed. This is true even with new Chandra observation, which provides newly the spatially resolved spectra. We have shown below with 3D modelling and the Chandra image that pure toroidal magnetic field and KED wind are incompatible with the Chandra observation.
dc.description5 pages, 6 figures, to appear in Proceedings of IAU 8th Asican Pacific Regional Metting Vol. II
dc.identifierhttps://arxiv.org/abs/astro-ph/0207437
dc.identifierhttp://arxiv.org/abs/astro-ph/0207437
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/4739
dc.subjectAstrophysics
dc.titlePulsar Wind Nebulae and Particle Acceleration in the Pulsar Magnetosphere
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