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Low–Mass He WDs and Millisecond Pulsars Age Determination

Published online by Cambridge University Press:  12 April 2016

J. Antipova ,
Ene Ergma  and
M. J. Sarna
J. Antipova
Affiliation:
Department of Physics, University of Tartu, Ülikooli 18, EE2400 Tartu, Estonia
Ene Ergma
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 the formation of a millisecond binary pulsar (MBP) 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 red giant (Bhattacharaya & van den Heuvel 1991). In this paper we shall discuss the cooling properties of the helium white dwarfs (WD) in short orbital period MBP systems PSR J0437–4715, PSR J0751+1807 and PSR J1012+5307, without referring to the rotational history of neutron stars (NS).

Below we discuss observational data for several system for which the results of our calculations (Sarna, Antipova, & Muslimov 1998; Sarna, Ergma, & Antipova 1999) may be applied, by taking into account the orbital parameters of the system, the pulsar spin-down time, and the WD cooling time-scale.

Type
Part 9. Population and Neutron Star Properties
Information
International Astronomical Union Colloquium , Volume 177: Pulsar Astronomy - 2000 and Beyond , 2000 , pp. 631 - 632
Copyright
Copyright © Astronomical Society of the Pacific 2000

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