Astronomy and Astrophysics – Astronomy
Scientific paper
Oct 1995
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995mnras.276.1320t&link_type=abstract
Monthly Notices of the Royal Astronomical Society, Volume 276, Issue 4, pp. 1320-1326.
Astronomy and Astrophysics
Astronomy
5
Binaries: Close, Stars: Evolution, Pulsars: Individual: Psr 1913+16, Pulsars: Individual: Psr 1534+12
Scientific paper
The relativistic binary pulsars PSR 1913+16 and 1534+12 are unique among binary pulsars in that their masses are accurately known as a result of studying general relativistic effects arising from their extremely short orbital periods (<~10h) and stable pulse periods. In order to produce such binary pulsar systems, the progenitor systems must have lost significant mass and angular momentum via a phase of common-envelope evolution. The survival of such systems requires that they must have, at one time, been long-period (~2-3 yr) binaries. Conservative thermal time-scale mass transfer is ruled out as a mechanism for producing such long-period binaries for the progenitors of these relativistic binary pulsars. We develop evolutionary scenarios for PSR 1913+16 and 1534+12 which provide an understanding of the fact that the observed pulsars are, respectively, the more and less massive neutron stars in their system.
Taam Ronald E.
Terman James Lewis
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