Statistical Properties of High-Energy Radiation from Young Pulsars

Details Statistical Properties of High-Energy Radiation from Young Pulsars Statistical Properties of High-Energy Radiation from Young Pulsars

Jun 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006apj...643.1130j&link_type=abstract

The Astrophysical Journal, Volume 643, Issue 2, pp. 1130-1138.

Statistics

12

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

Scientific paper

We study the statistical properties of young pulsars with ages of <=106 yr using the Monte Carlo method on the frame of a revised outer gap model. In our simulations, we first compare the simulated radio-loud pulsars with the observed ones in the ATNF Pulsar Catalogue, in which nine radio surveys are included. On the basis of consistency between the simulated and the observed young pulsars, we further simulate possible γ-ray pulsars based on our outer gap model. In this model, geometric effects have been taken into account, and the high-energy radiation of a pulsar depends on period (P), magnetic field (B), and magnetic inclination angle (α). We take the γ-ray beaming selection effects into account and study the statistical properties of γ-ray pulsars with energy fluxes above the detectable threshold fluxes. For the EGRET detector, we predict that there may be ~8 radio-loud and ~24 radio-quiet γ-ray pulsars if we take the neutron star birthrate to be 1.5 per century. For GLAST, we expect ~78 and ~740 radio-loud and radio-quiet γ-ray pulsars. Most of the young γ-ray pulsars are concentrated at the Galactic plane. We compared the energy fluxes of the simulated γ-ray pulsars with those of low-latitude unidentified EGRET γ-ray sources, indicating that the majority of these unidentified sources have pulsar origin.

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