Gamma-ray luminosity properties of gamma-ray pulsars

Details Gamma-ray luminosity properties of gamma-ray pulsars Gamma-ray luminosity properties of gamma-ray pulsars

Jan 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005a%26a...429..489z&link_type=abstract

Astronomy and Astrophysics, v.429, p.489-495 (2005)

Statistics

5

Gamma-Rays: Theory, Stars: Pulsars: General, Stars: Neutron, Stars: Statistics

Scientific paper

Based on a new self-consistent outer gap model, we statistically study luminosity properties of γ-ray pulsars with ages of ≤2× 107 yr in the Galaxy as well as those with ages of ≤5× 106 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, Lγ, and pulsar spin-down power, Lsd, can be expressed as Lγ ∝ Lδsd, 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 |b|≤5°, and δ increases by a factor of ˜2 at the range of | b |= 5°-10° relative to δ at | b | ≤5°, 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.

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