Volume 454, Number 2, August I 2006
APEX Special Booklet
|Page(s)||537 - 542|
|Section||Stellar structure and evolution|
|Published online||11 July 2006|
Non-thermal pulsed X-ray emission from rotation-powered pulsars
National Astronomical Observatories/Yunnan Observatory, Chinese Academy of Sciences, PO Box 110, Kunming, China e-mail: firstname.lastname@example.org
2 Department of Physics, Yunnan University, Kunming, China
Accepted: 28 March 2006
We study the properties of the pulsed component of hard (>2 keV) X-ray emission from pulsars based on the new version of the outer-gap model proposed by Zhang et al. (2004). In this outer-gap model, high-energy photons emitted by relativistic charged particles produce e pairs through magnetic-pair production on their way from the outer gap to the neutron-star surface, and these pairs produce the bulk of pulsed X-rays by the synchrotron radiation. The X-ray luminosity of rotation-powered pulsars is a function not only of the period and magnetic field strength, but also of the magnetic inclination angle. Application of this model to the observed pulsed X-ray emission of normal pulsars by ASCA shows a better consistence. Further, the inclination angles of these pulsars are estimated using the observed X-ray data, and the predicted conversion efficiencies of high-energy γ-rays for seven confirmed γ-ray pulsars are consistent with the observed data.
Key words: pulsars: general / radiation mechanisms: non-thermal / X-rays: stars
© ESO, 2006
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.