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Neutron Star Formation by Collapse of White Dwarfs

Published online by Cambridge University Press:  12 April 2016

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

Abstract.

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Mass-accreting carbon-oxygen white dwarfs become thermally and dynamically unstable when they reach high enough central densities. Carbon ignition at the star’s center likely propagates subsonically and, in the case of an initially solid core, leads to collapse if the rate of increase of the core’s mass is sufficiently fast. Recent results indicate, however, that solidification of the core induces carbon-oxygen separation. The central regions are then made of pure oxygen while carbon is rejected to lower-density layers. Carbon ignition happens only after neutronization of the central (oxygen) regions. Collapse to a neutron star is then independent from the rate of mass increase and the only possible restrictions are set by the behaviour of the outer, accreted layers. X-ray sources, pulsars and Type I supernovae are likely outcomes of this process.

Type
IX. Supernovae
Information
International Astronomical Union Colloquium , Volume 58: Stellar Hydrodynamics , August 1980 , pp. 595 - 600
Copyright
Copyright © Reidel 1980

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