A New Asymmetric Emission Model for Accreting X-ray Pulsars

Details A New Asymmetric Emission Model for Accreting X-ray Pulsars A New Asymmetric Emission Model for Accreting X-ray Pulsars

Aug 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999icrc....4..123l&link_type=abstract

Proceedings of the 26th International Cosmic Ray Conference. August 17-25, 1999. Salt Lake City, Utah, USA. Under the auspices o

Physics

Scientific paper

A new model for pulsed emission from rotating accreting neutron stars is presented. This model considers asymmetrically paralled accretion columns extending above the neutron star polar caps. The particular geometry which is modelled is expected to result from an accretion ow from a disk onto the magnetosphere of the pulsar, and is described by a few basic parameters. The model uses the local emission derived from published magnetic-radiative transfer calculations as input. The output is the x-ray pulse shape at various energies, as a function of the parameters of the polar accretion ow geometry. The emission is generally of a fan-beam type, which results from emission by the sides of the accretion column.

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