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Collapse of Accreting White Dwarf to Form a Neutron Star

Published online by Cambridge University Press:  12 April 2016

Ken’ichi Nomoto ,
Shigeki Miyaji ,
Daiichiro Sugimoto  and
Koichi Yokoi
Ken’ichi Nomoto
Affiliation:
Department of Physics, Ibaraki University, Mito 310, Japan
Shigeki Miyaji
Affiliation:
Deparment of Earth Science and Astronomy, College of General Education, University of Tokyo, Tokyo 153, Japan
Daiichiro Sugimoto
Affiliation:
Deparment of Earth Science and Astronomy, College of General Education, University of Tokyo, Tokyo 153, Japan
Koichi Yokoi
Affiliation:
Science and Engineering Research Laboratory, Waseda University, Tokyo 160, Japan

Abstract

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In a close binary system with a primary star in the mass range 8-12 M⊙, the primary star leaves a white dwarf composed of 16O, 20Ne, and 24Mg as a result of mass exchange. When the companion star, fills its Roche lobe, overflowing matter accretes onto the white dwarf. We have computed the evolution of such an accreting O-Ne-Mg white dwarf and found that electron captures on 24Mg and 20Ne trigger the collapse when the mass reaches 1.38 M⊙. As a result of the collapse, oxygen begins to deflagrate but the effects of electron captures dominate over the oxygen deflagration. The white dwarf collapses to form a neutron star.

Type
Colloquium Session I
Information
International Astronomical Union Colloquium , Volume 53: White Dwarfs and Variable Degenerate Stars , August 1979 , pp. 56 - 60
Copyright
Copyright © The University of Rochester 1979

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