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Formation of Luminous Contact Binaries by Rapid Accretion onto White Dwarfs

Published online by Cambridge University Press:  14 August 2015

Ken'Ichi Nomoto ,
Kyoji Nariai  and
Daiichiro Sugimoto
Ken'Ichi Nomoto
Affiliation:
*Department of Physics, Ibaraki University
Kyoji Nariai
Affiliation:
*Tokyo Astronomical Observatory, University of Tokyo
Daiichiro Sugimoto
Affiliation:
**College of General Education, University of Tokyo

Extract

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During the evolution of a close binary system, there is a phase of mass exchange between its component stars. When the mass-losing star is an evolved star off the main sequence, the mass exchange is very rapid. Its rate may well exceed the critical accretion rate corresponding to the Eddington limit of the mass accreting star. Effects of such a rapid accretion were studied for the mass-accreting main-sequence stars (Flannery and Ulrich 1977; Kippenhahn and Mayer-Hofmeister 1977; Neo et al. 1977). The mass-accreting stars become quickly overluminous and their radii increase even to a red-giant size as mass is accumulated. Then the both component stars will fill their Roche lobes to form a contact binary system.

Type
III. Mass Transfer and Mass Loss - Theory
Information
Symposium - International Astronomical Union , Volume 88: Close Binary Stars: Observations and Interpretation , 1980 , pp. 139 - 143
Copyright
Copyright © Reidel 1980 

References

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