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Plasma Distribution Functions in Accretion onto Neutron Stars

Published online by Cambridge University Press:  25 April 2016

N.F. Cramer
N.F. Cramer*
Affiliation:
School of Physics, The University of Sydney
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Extract

In the usual model of discrete cosmic X-ray sources, it is assumed that a massive star loses matter to a companion neutron star, either through a stellar wind, or by means of Roche lobe overflow into an accretion disk around the neutron star (Pines 1980). The irifalling matter becomes ionized and is channelled along the magnetic field lines of the neutron star, so that it is accreted onto the star in a very small region at the magnetic polar caps. The physical conditions at these points are assumed to be: magnetic field B ~ 1012 G, plasma temperature ~107-108 K, and infall plasma velocity ~ 0.3 c-0.5 c.

Type
Contributions
Information
Publications of the Astronomical Society of Australia , Volume 4 , Issue 4 , 1982 , pp. 370 - 371
Copyright
Copyright © Astronomical Society of Australia 1982

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