Population Statistics Study Of Normal Isolated, Radio And Gamma-ray Pulsars From The Galactic Plane

Details Population Statistics Study Of Normal Isolated, Radio And Gamma-ray Pulsars From The Galactic Plane Population Statistics Study Of Normal Isolated, Radio And Gamma-ray Pulsars From The Galactic Plane

Sep 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006head....9.0771g&link_type=abstract

American Astronomical Society, HEAD meeting #9, #7.71; Bulletin of the American Astronomical Society, Vol. 38, p.361

Astronomy and Astrophysics

Astrophysics

Scientific paper

We present results of our pulsar population synthesis of ordinary isolated pulsars in the Galactic plane. Over the past several years, a program has been developed to simulate pulsar birth, evolution and emission using Monte Carlo techniques. We model the spatial distribution of pulsars by assuming that they start with a random kick velocity and then evolve through the Galactic potential set forth in Dehnen & Binney (1996). We explore both uniform and non-uniform spatial birth distributions within the Galactic plane. We assume that pulsars are standard candles and invoke a new relationship between core and cone emission suggested by recent studies, which we also apply to millisecond pulsars. From our studies of radio pulsars that have clearly identifiable core and cone components, in which we fit the polarization sweep as well as the pulse profiles in order to constrain the viewing geometry, we develop a model describing the ratio of radio core-to-cone peak fluxes. In this model, short period pulsars are more cone-dominated than in our previous studies. We use both a low and high altitude slot gap model for describing the gamma-ray emission. We also include gamma-ray emission from an outer-gap model to compare the statistics of radio-loud and radio-quiet gamma-ray pulsars on the same footing as pulsars from our slot gap, polar cap model. We present the preliminary results of our recent study and the implications for observing these pulsars with GLAST and AGILE.
We express our gratitude for the generous support of the Michigan Space Grant Consortium, of Research Corporation (CC5813), of the National Science Foundation (REU and AST-0307365) and the NASA Astrophysics Theory Program.

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