Evolution of compact binary systems with X-ray heating

Details Evolution of compact binary systems with X-ray heating Evolution of compact binary systems with X-ray heating

Dec 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991apj...383..739h&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 383, Dec. 20, 1991, p. 739-744.

Physics

53

Radiant Heating, Stellar Evolution, Stellar Physics, X Ray Binaries, X Ray Irradiation, Accretion Disks, Mass Transfer, Roche Limit, Stellar Motions, Stellar Systems

Scientific paper

Results of calculations of the evolution of low-mass X-ray binary systems with the inclusion of heating of the secondary star by the X-radiation from the primary are presented. The secondary is assumed to be nonsynchronously rotating with the orbit, so that the X-ray heating may be taken to be approximately uniform over its surface. The evolution of binary systems with secondary stars of initial mass 0.4 and 1 solar mass is computed. The expansion of the secondary due to the X-ray heating is found to cause high rates of mass loss from the star for significant intervals of time, for both values of the secondary mass. The evolution of the two binary systems under consideration are characterized by very high initial mass-loss rates during the first expansion phase, followed by a decreasing mass-loss rate during the second of the expansion phases.

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