Astrophysics and Space Science

, Volume 131, Issue 1, pp 675–679

Mass loss and shell masses of close binary stars

Authors

  • V. G. Karetnikov
    • Astronomical Department of the Odessa State University
Related Objects

DOI: 10.1007/BF00668156

Cite this article as:
Karetnikov, V.G. Astrophys Space Sci (1987) 131: 675. doi:10.1007/BF00668156
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Abstract

From the values of period changes for 6 close binary stars the mass transfer rate was calculated. Comparing these values Mt with the values of shell masses Msh, the expression
$$lg \dot M_t = \begin{array}{*{20}c} {4.24} \\ { \pm 24} \\ \end{array} + \begin{array}{*{20}c} {0.63} \\ { \pm 6} \\ \end{array} lg M_{sh} $$

Was derived. The analysis of this expression points out the initial character of the outflow of matter, and one may determine the time interval of the substitution of the shell matter. So one may conclude that for a certain mass transfer rate, a certain amount of matter accumulates in the nearby regions of the system.

The study of orbital period changes of close binary stellar systems led to the idea that these secular and irregular changes are due to the mass loss and to the redistribution of masses in a close binary. Secular changes of orbital periods are known for approximately 400 eclipsing binary stars. For many stars, including cataclysmic binaries, irregular period changes are known. Thus, the mass loss and the matter redistribution in close binaries are often observed phenomena.

Copyright information

© D. Reidel Publishing Company 1987