A population synthesis study of low-mass X-ray binary systems

Details A population synthesis study of low-mass X-ray binary systems A population synthesis study of low-mass X-ray binary systems

Jul 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996mnras.281..552t&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 281, Issue 2, pp. 552-564.

Astronomy and Astrophysics

Astronomy

14

Binaries: Close, Stars: Evolution, Stars: Neutron

Scientific paper

The origin of low-mass X-ray binary systems from the helium star-main-sequence binary remnants of a common-envelope phase is studied. Using a statistical Monte Carlo approach, the evolution of an initial distribution of zero-age binaries is followed from the main sequence through a phase of common-envelope evolution and subsequent supernova explosion of the helium star. The resultant population of low-mass main-sequence stars (<~3 M_) with a neutron star companion is studied as a function of the kick velocity associated with the possible asymmetry of the supernova explosion, the efficiency of mass ejection during the common-envelope phase, the minimum mass for evolution to a neutron star and the mass distribution of the secondary components in the system. A comparison of the results with the observed low-mass X-ray binary system population suggests that kick velocities are required. For an average kick velocity of ~450 km s^-1, as inferred from the radio pulsar distribution, birth rates in the range ~3x10^-6-10^-5 yr^-1 are indicated for efficiencies of the mass ejection process during the common-envelope phase of 0.25-1. The implications of the results for the general population of low-mass X-ray binaries, and for the formation of Her X-1 type systems and long-period detached systems similar to PSR 1820-11, are briefly discussed.

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