Pulsar wind nebulae: theoretical aspects and observational constraints

Abstract

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. The low magnetic field is consistent with models in which the nebulae are created by a shocked pulsar wind.