Abstract
The evolution of low-mass X-ray binary systems is calculated with the inclusion of heating of the secondary star by the X-radiation from the primary. 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. Due to the shadowing effect of a postulated accretion disk, only a portion of the X-ray flux reaches the secondary star. The evolution of binary systems with secondary stars of initial mass 0.4 and 1 M ⊙ is computed
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