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: email@example.com
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
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