Evolution of Massive Close Binaries. II: The Post X-Ray Binary Stage: Origin of Run-away and Binary Pulsars

TLDR: In this paper, the further evolution of a massive X-ray binary consisting of a compact object and an OB supergiant is outlined, and the probability for the generation of binary pulsars is very low; in most cases the system is disrupted during the supernova explosion.

Abstract: 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 22.5M⊙+2M⊙. 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 ofi=40° may be derived. The probability for the generation of binary pulsars is very low; in most cases the system is disrupted during the supernova explosion.