HEAD 2000, November 2000
Session 33. Isolated Pulsars
Display, Thursday, November 9, 2000, 8:00am-6:00pm, Bora Bora Ballroom

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[33.17] Galactic Population of Radio and Gamma-Ray Pulsars

P.L. Gonthier, J. Berrier (Department of Physics and Engineering), M.S. Ouellette (Michigan State University, Physics and Astronomy Department), S. O'Brien (University of Notre Dame, Department of Physics), A.K. Harding (NASA - Goddard Space Flight Center)

We simulate the characteristics of the Galactic population of radio and gamma-ray pulsars using Monte Carlo techniques. At birth, neutron stars are spatially distributed with supernova-kick velocities in the Galactic disk and randomly dispersed in age back to 109 years. They are evolved in the Galactic gravitational potential to the present time. From a radio luminosity model, the radio flux is filtered through a selected set of radio-survey parameters. Using the features of recent polar cap acceleration models invoking space-charge-limited flow, a pulsar death region further attenuates the population and radio-loud pulsars are assigned gamma-ray luminosities. In this paper, we will discuss detailed comparisons between the characteristics of calculated pulsars and those of observed pulsars. We will present predictions of the number of radio-loud, gamma-ray pulsars observed by EGRET and GLAST.

This work was supported in part by the NSF grant no. SAA 9876670, NSF-REU, Research Corporation, and Michigan Space Grant Consortium.

The author(s) of this abstract have provided an email address for comments about the abstract: gonthier@physics.hope.edu

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