Evolution of massive close binaries. II - The POST X-ray binary stage: Origin of run-away and binary pulsars

Details Evolution of massive close binaries. II - The POST X-ray binary stage: Origin of run-away and binary pulsars Evolution of massive close binaries. II - The POST X-ray binary stage: Origin of run-away and binary pulsars

Aug 1975

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975ap%26ss..36..219d&link_type=abstract

Astrophysics and Space Science, vol. 36, Aug. 1975, p. 219-225. Fonds National de la Recherche Scientifique

Astronomy and Astrophysics

Astronomy

48

Binary Stars, Pulsars, Stellar Evolution, Supergiant Stars, X Ray Sources, B Stars, Black Holes (Astronomy), Neutron Stars, O Stars, Stellar Mass, Stellar Mass Ejection

Scientific paper

The further evolution of a massive X-ray binary consisting of a compact object and an OB supergiant is outlined. The supergiant exceeds its critical Roche lobe and a second stage of mass transfer starts. The remnant of the mass losing star - a pure helium star - develops a collapsing iron core and finally undergoes a supernova explosion. If the compact companion is a black hole the system remains bound; if the compact companion is a neutron star the system is disrupted unless an extra kick allowing an asymmetric explosion is given. Computations were performed for the massive binary 22.6 M®+ 2 M0. The possible final evolutionary products are: (1) a black hole and a compact object, in a binary system, (2) two run-away pulsars, (3) a binary pulsar. As final parameters for the described system the eccentricity and period for the recently discovered binary pulsar 1913+ 16 may be found. An orbital inclination of i= 400 may be derived. The probability for the generation of binary pulsars is very low; in most cases the system is disrupted during the super- nova explosion

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