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Millisecond Pulsar Formation and Evolution

Published online by Cambridge University Press:  04 August 2017

E.P.J. van den Heuvel
E.P.J. van den Heuvel*
Affiliation:
Astronomical Institute University of Amsterdam, Roetersstraat 15, 1018 WB Amsterdam, The Netherlands

Abstract

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The evolutionary history of binary radio pulsars, including the two millisecond binary pulsars, is reviewed. There are two groups of binary pulsars, the PSR 1913+16-group, which descended from massive X-ray binaries, and the PSR 1953+29-group, which descended from fairly wide low-mass X-ray binaries. The neutron stars in the second group probably formed by the accretion-induced collapse of a massive white dwarf. The companion stars in both groups of systems are expected to be dead stars, i.e. white dwarfs or neutron stars.

The large total number of millisecond binary pulsars in the galaxy (∼ 104), indicates that magnetic fields of neutron stars do not decay below a value of order 109 G. Possible explanations for this phenomenon are discussed.

Coalescence with a close degenerate companion provides a viable model for the formation of the single millisecond pulsar.

Type
IV. Neutron Stellar Evolution
Information
Symposium - International Astronomical Union , Volume 125: The Origin and Evolution of Neutron Stars , 1987 , pp. 393 - 406
Copyright
Copyright © Reidel 1987 

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