Soft X-ray transients and the evolution of low mass X-ray binaries

Details Soft X-ray transients and the evolution of low mass X-ray binaries Soft X-ray transients and the evolution of low mass X-ray binaries

Jan 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987a%26a...171..140h&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 171, no. 1-2, Jan. 1987, p. 140-144.

Astronomy and Astrophysics

Astrophysics

22

Radiant Flux Density, Stellar Evolution, Stellar Mass, Variable Stars, X Ray Binaries, Stellar Models

Scientific paper

The conditions under which low-mass X-ray binaries are likely to appear as soft X-ray transients are investigated, using the X-ray illumination model developed in an earlier paper (Hameury et al., 1986). It is shown that transient behavior is possible for a narrow range of systems having evolved companions and is likely for all systems with quasi-main sequence companions having binary periods not greater than 2 hr. This, together with the 'period gap' beteen 2 and 3 hr likely for these systems, probably explains the absence of low-mass X-ray binaries with observed periods of less than 2.9 hr. A transient behavior at larger periods is only possible if the average accretion rate corresponds to that given by gravitational radiation losses, i.e., if the usual driving mechanisms (e.g., magnetic braking) are temporarily inefficient, as observed.

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