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Helium white dwarf cooling in PSR J0751+1807 and PSR J1012+5307

Published online by Cambridge University Press:  12 April 2016

Ene Ergma ,
J. Antipova  and
M. J. Sarna
Ene Ergma
Affiliation:
Department of Physics, University of Tartu, Ülikooli 18, EE2400 Tartu, Estonia
J. Antipova
Affiliation:
Department of Physics, University of Tartu, Ülikooli 18, EE2400 Tartu, Estonia
M. J. Sarna
Affiliation:
N. Copernicus Astronomical Center, Polish Academy of Sciences, ul. Bartycka 18, 00-716 Warsaw, Poland

Extract

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It is accepted that formation of a binary millisecond (or recycled) pulsar with a low–mass companion may be explained as the end–point of close binary evolution in which an old pulsar is spun–up by accretion from the secondary (Alpar et al., 1982). After detachment from the Roche lobe, the pulsar spin period starts to change due to magneto–dipole radiation and the white dwarf begins to cool down. In this paper we shall discuss the cooling history of helium core low–mass white dwarfs in the short orbital period millisecond binary pulsars PSR J0751+1807 and PSR J1012+5307 (Ergma, Sarna, & Antipova 1999).

Type
Part 9. Population and Neutron Star Properties
Information
International Astronomical Union Colloquium , Volume 177: Pulsar Astronomy - 2000 and Beyond , 2000 , pp. 637 - 640
Copyright
Copyright © Astronomical Society of the Pacific 2000

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