Volume 429, Number 2, January II 2005
|Page(s)||489 - 495|
|Section||Galactic structure, stellar clusters, and populations|
|Published online||17 December 2004|
Gamma-ray luminosity properties of gamma-ray pulsars
National Astronomical Observatories/Yunnan Observatory, Chinese Academy of Sciences, PO Box 110, Kunming, PRC, PR China e-mail: firstname.lastname@example.org
2 Department of Physics, Yunnan University, Kunming, PR China
Accepted: 30 August 2004
Based on a new self-consistent outer gap model, we statistically study luminosity properties of γ-ray pulsars with ages of ≤ yr in the Galaxy as well as those with ages of ≤ yr in the Gould belt using a Monte Carlo method, where the γ-ray beaming effect has been included. Generally, the relation between γ-ray luminosity, , and pulsar spin-down power, Lsd, can be expressed as , where δ is a parameter that depends on the galactic latitude and the γ-ray threshold. For a given γ-ray threshold (for example, the EGRET threshold or GLAST threshold), the parameter δ is an increasing function of the galactic latitude. For the EGRET threshold, δ changes smoothly with the galactic latitude. For the GLAST threshold, however, δ has a minimum at , and δ increases by a factor of ~2 at the range of relative to δ at , and then increases smoothly as the galactic latitude further increases. The reason for this is that high galactic latitude γ-ray pulsars are dominated by mature pulsars. In fact, the ratio of γ-ray pulsars with their ages of >106 yr to all simulated γ-ray pulsars also increases with the galactic latitude. For the γ-ray pulsars produced in a fixed range of galactic latitude, the parameter δ increases slightly with the sensitivity of γ-ray detector.
Key words: gamma-rays: theory / stars: pulsars: general / stars: neutron / stars: statistics
© ESO, 2005
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