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Numerical Simulation of Mass Transfer and Accretion Disc Flow in Binary Systems

Published online by Cambridge University Press:  14 August 2015

D. N. C. Lin  and
J. E. Pringle
D. N. C. Lin
Affiliation:
Institute of Astronomy, Madingley Road, Cambridge CB3 OHA, England
J. E. Pringle
Affiliation:
Institute of Astronomy, Madingley Road, Cambridge CB3 OHA, England

Abstract

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A numerical simulation of equilibrium gas flow in a binary system is presented for the case in which an accretion disc forms around the accreting star (primary). Preliminary results are shown for the mass ratios 0.4, 1.0 and 2.5. Two main conclusions are reached. First, the accretion disc is quite well defined and is comparable in size to the Roche lobe of the primary. Second, all but a few per cent of the mass transferred is accreted by the primary.

Type
Research Article
Information
Symposium - International Astronomical Union , Volume 73: Structure and Evolution of Close Binary Systems , 1976 , pp. 237 - 252
Copyright
Copyright © Reidel 1976 

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