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Collapse of White Dwarfs in Close Binary Systems

Published online by Cambridge University Press:  12 April 2016

R. Canal  and
J. Isern
R. Canal
Affiliation:
Departamento de Fisica de la Tierra y del Cosmos, Universidad de Barcelona
J. Isern
Affiliation:
Departamento de Fisica de la Tierra y del Cosmos, Universidad de Barcelona

Extract

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The presence of neutron stars in close binary systems, shown by the pulsating X-ray sources, poses the problem of their origin. In the case of the low-mass (M1 + M2 ≤ 5 M⊙) X-ray binaries, the neutron star might have originated from a massive white dwarf, driven over the Chandrasekhar limit by mass transfer (Schatzman 1974). A similar scenario had been put forward by Whelan and Iben (1973) for type I supernovae. To solve the problem of the very low eccentricities observed for the orbits, and to facilitate keeping the system bound after neutron star formation, Canal and Schatzman (1976) suggested a non explosive collapse of the white dwarf to a neutron star. The occurence of this kind of collapse depended on the possibility of avoiding thermonuclear ignition by means of neutronization. Since there is a density interval where the electron captures on carbon go faster than the pycnonuclear reactions, just above the critical density for the beginning of the collapse, there seemed also to be a chance of escape from thermonuclear runaway. A closer examination of this picture leads, however, to significant changes.

Type
Colloquium Session I
Information
International Astronomical Union Colloquium , Volume 53: White Dwarfs and Variable Degenerate Stars , August 1979 , pp. 52 - 55
Copyright
Copyright © The University of Rochester 1979

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