Abstract
The response of a 1.25 solar mass secondary ZAMS star to the low-density, high-entropy conditions within the common envelope of a red giantlike configuration is numerically investigated in order to examine the state of the star on its emergence from the common-envelope stage. The results demonstrate that such a star accumulates little matter, typically less than 0.01 solar mass, after a long adiabatic accretion phase followed by a brief, nearly adiabatic Roche-lobe overflow phase. The evolution time scale for the common-envelope phase is rapid, and the duration of the common-envelope phase is 400-4000 yr. It is expected that the envelope of the secondary would significantly depart from a thermal equilibrium state on its emergence from the common-envelope phase. Once the common envelope is ejected, the thermal relaxation time scale of the disturbed outer envelope layer of the secondary is found to be about 10,000 yr.
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