Mass loss from OB supergiants in X-ray binary systems

Details Mass loss from OB supergiants in X-ray binary systems Mass loss from OB supergiants in X-ray binary systems

Oct 1975

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975nyasa.262..379a&link_type=abstract

(AAS, American Physical Society, and New York Academy of Sciences, Texas Symposium on Relativistic Astrophysics, 7th, Dallas, Te

Astronomy and Astrophysics

Astrophysics

1

Binary Stars, Mass Flow Rate, O Stars, Roche Limit, Supergiant Stars, X Ray Stars, Astronomical Models, B Stars, Mass Transfer, Radiative Transfer, Stellar Winds, Time Dependence

Scientific paper

The characteristics of an OB supergiant overflowing its Roche lobe are studied on the basis of a model for time-dependent hydrodynamics and radiation transport in a spherically symmetric problem geometry. A study of the hydrodynamics of material near the inner Lagrangian point indicates that large-amplitude variations in the mass transfer occurs when the stellar surface is close enough to the saddle in the gravitational potential to provide sufficient mass transfer to power a compact X-ray source. For a particular model of the Cygnus X-1 binary system, calculations show that the material passing through the inner Lagrangian point has a temperature of about 2 eV and a Mach number of 4 or 5.

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