Polar CAP models of gamma-ray pulsars: Emision from single poles of nearly aligned rotators

Details Polar CAP models of gamma-ray pulsars: Emision from single poles of nearly aligned rotators Polar CAP models of gamma-ray pulsars: Emision from single poles of nearly aligned rotators

Jul 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...429..325d&link_type=abstract

The Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 429, no. 1, p. 325-330

Astronomy and Astrophysics

Astrophysics

71

Gamma Ray Beams, Pulsars, Rotating Spheres, Gamma Ray Observatory, Magnetic Poles, Polar Regions, Radio Bursts, Stellar Models, X Ray Stars

Scientific paper

We compare a new Monte Carlo simulation of polar cap models for gamma-ray pulsars with observations of sources detected above 10 MeV by the Compton Observatory (CGRO). We find that for models in which the inclination of the magnetic axis is comparable to the angular radius of the polar cap, the radiation from a single cap may exhibit a pusle with either a single broad peak as in PSR 1706-44 and PSR 1055-52, or a doubly peaked profile comparable to those observed from the Crab, Vela and Geminga pulsars. In general, double pulses are seen by observers whose line of sight penetrates into the cap interior and are due to enhanced emission near the rim. For cascades induced by culvature radiation, increased rim emission occurs even when electrons are accelerated over the entire cap, since electrons from the interior escape along magnetic field lines with less curvature and hence emit less radiation. However, we obtain better fits to the duty cycles of observed profiles if we make the empirical assumption that acceleration occurs only near the rim. In either case, the model energy spectra are consistent with most of the observed sources. The beaming factors expected from nearly aligned rotators, based on standard estimates for the cap radius, imply that their luminosities need not be as large as in the case of orthogonal rotators. However, small beam angles are also a difficutly with this model because they imply low detection probablities. In either case the polar cap radius is a critical factor, and in this context we point out that plasma loading of the field lines should make the caps larger than the usual estimates based on pure dipole fields.

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