On the X-ray jets in pulsar wind nebulae

Research output: Chapter in Book/Report/Conference proceedingChapterpeer-review

Abstract

The origin of the X-ray jet in the inner Crab nebula and other pulsar wind nebulae is discussed. A jet may be formed in axisymmetric, magnetized pulsar winds and the jet luminosity scales relative to the total as gamma0*(sigma0)(-4/3), where gamma0 is the Lorentz factor at the base of the flow and sigma0 the ratio of Poynting flux to particle energy output. A jet with reasonable luminosity may be formed in the Crab pulsar wind if only gamma0 * sigma0 >> 100. This means that the wind is much more mass loaded than previously believed. Another possibility is discussed, namely, that the jet is formed beyond the termination shock. It is argued that the shock shape should be highly non-spherical, the shock being much closer to the pulsar near the axis than at the equator. Therefore the jet may look as if it originates directly from the pulsar.
Original languageEnglish
Title of host publicationNeutron Stars in Supernova Remnants
EditorsPatrick O. Slane, Bryan M. Gaensler
Place of PublicationSan Francisco
Pages91-94
ISBN (Electronic)9781583816073
StatePublished - 2002

Publication series

NameASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES

Fingerprint

Dive into the research topics of 'On the X-ray jets in pulsar wind nebulae'. Together they form a unique fingerprint.

Cite this