Pulsar Wind Nebulae: Theoretical Aspects and Observational Constraints

Astrophysics, abstract
astro-ph/0301370

From: Roger A. Chevalier <rac5x@karma.astro.virginia.edu>

Date: Fri, 17 Jan 2003 22:08:47 GMT   (27kb)

Authors:
Roger A. Chevalier

Comments: 9 pages, to appear in “High Energy Studies of Supernova Remnants and
Neutron Stars” (COSPAR 2002), Advances in Space Research

Of the known pulsar wind nebulae, 8 are good candidates for being in the
early stage of evolution where the wind nebula is interacting with the freely
expanding supernova ejecta. Several of these have been identified with
historical supernovae. Although the identification of SN 1181 with 3C 58 has
been thought to be relatively secure, the large size of the nebula, the amount
of swept up mass, and the internal energy indicate a larger age. For G11.2-0.3,
the nebular size and internal energy are consistent with the identification
with the possible supernova of 386. Although the Crab Nebula appears to have
approximate energy equipartition between particles and the magnetic field, the
nebulae 3C 58 and MSH 15-52 appear to be particle dominated. %Pulsar wind
nebulae can be generally described by a model %with a shocked pulsar wind, but
there appears to be considerable diversity %among objects. The low magnetic
field is consistent with models in which the nebulae are created by a shocked
pulsar wind.

References and citations for this submission:

SLAC-SPIRES HEP (refers to ,
cited by, arXiv reformatted)