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Gravitational Collapse of Mass-Accreting White Dwarfs

Published online by Cambridge University Press:  12 April 2016

J. Isern ,
R. Canal ,
D. García ,
M. Hernanz  and
J. Labay
J. Isern
Affiliation:
Centre d’Estudis Avançats de Blanes, CSIC 17300 Blanes (Girona), Spain
R. Canal
Affiliation:
Departament de Física de l’Atmosfera, Astronomia i AstrofisicaUniversitat de Barcelona, 08028 Barcelona, Spain
D. García
Affiliation:
Universitat Politècnica de Catalunya 08028 Barcelona, Spain
M. Hernanz
Affiliation:
Universitat Politècnica de Catalunya 08028 Barcelona, Spain
J. Labay
Affiliation:
Departament de Física de l’Atmosfera, Astronomia i AstrofisicaUniversitat de Barcelona, 08028 Barcelona, Spain

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Massive star (M ≥ 10 M ) core collapse is the standard mechanism for neutron star formation (see Brown 1988 for a recent review). It has long been realized (see, for instance, van den Heuvel 1988, and references therein) that the neutron stars found in different types of binary systems cannot come from such a standard mechanism. Those systems include wide binary radio pulsars, millisecond pulsars (not in wide binaries), galactic bulge X–ray sources (including QPO’s), type I X–ray burst sources and X–ray transients, andγ–ray sources. Formation of those neutron stars is now widely attributed to the gravitational collapse of a white dwarf, growing above Chandrasekhar’s limit by mass accretion from the current neutron star’s companion in the binary system (Canal and Schatzman 1976; Canal and Isern 1979; Canal, Isern, and Labay 1980; Miyaji et al. 1980). Mass growth up to dynamical instability means that both explosive ejection of the accreted layers and explosive disruption of the whole star must be avoided. The former is associated with the nova phenomenon. The latter, with the occurrence of type I supernovae.

Type
Research Article
Information
International Astronomical Union Colloquium , Volume 114: White Dwarfs , 1989 , pp. 88 - 91
Copyright
Copyright © Springer-Verlag 1989

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