A possible detection mechanism for pre-low-mass X-ray binaries

Details A possible detection mechanism for pre-low-mass X-ray binaries A possible detection mechanism for pre-low-mass X-ray binaries

May 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002mnras.332..689b&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 332, Issue 3, pp. 689-696.

Astronomy and Astrophysics

Astronomy

7

Binaries: Close, Stars: Neutron, X-Rays: Stars

Scientific paper

This work presents a possible detection mechanism for close, detached, neutron star-red dwarf binaries, which are expected to be the evolutionary precursors of low-mass X-ray binaries (LMXBs). Although this pre-low-mass X-ray binary (pre-LMXB) phase of evolution is predicted theoretically, as yet no such systems have been identified observationally. The calculations presented here suggest that the X-ray luminosity of neutron star wind accretion in a pre-LMXB system can be expected to exceed the intrinsic X-ray luminosity of the red dwarf secondary star. Furthermore, the temperature of the radiation emitted from the neutron star wind accretion process is expected, within the confines of a reasonable set of conditions, to lie within the detection range of X-ray satellites. Sources with X-ray luminosities greater than that expected for a red dwarf star, but the positions of which coincide with that of a red dwarf star, are then candidate pre-LMXB systems. These candidate systems should be surveyed for the radial velocity shifts that would occur as a result of the orbital motion of a red dwarf star within a close binary system containing a high-mass compact object.

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