Structure and Evolution of X-Ray Heated Compact Binaries

Details Structure and Evolution of X-Ray Heated Compact Binaries Structure and Evolution of X-Ray Heated Compact Binaries

Sep 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993a%26a...277...81h&link_type=abstract

Astronomy and Astrophysics, Vol. 277, NO. 1/SEP(III), P. 81, 1993

Astronomy and Astrophysics

Astrophysics

46

Accretion, Accretion Discs - (Stars:) Binaries: General - X-Rays: Stars, Pulsars: Millisecond

Scientific paper

We study the effect of X-ray illumination of the secondary star in a close binary on its internal structure and on the evolution of the system. We take into account the fact that X-ray heating is non-spherical and show that this modifies the results obtained in models which assume spherically symmetric illumination. Our results suggest that the effects of X-ray heating have been largely overestimated in earlier papers. We also show that radiation-induced winds in LMXBs with orbital periods less than 10 hr cannot give mass transfer rates larger than about one tenth of the Eddington limit mass flux, making it unlikely that such self-sustained winds have a marked effect on LMXB evolution, contrary to the suggestion of Tavani (1991). We discuss the consequences of these results for proposed evolutionary schemes connecting low-mass X-ray binaries and millisecond pulsars.

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