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Binary Evolution in Stellar Systems∗

Published online by Cambridge University Press:  14 August 2015

R. H. Miller
R. H. Miller*
Affiliation:
Dept. of Astronomy, University of Chicago, Chicago, Ill., U.S.A.

Abstract

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Aarseth has shown by means of n-body calculations that, in star systems with a range of particle masses, the most massive stars quickly form a binary which soon takes up a large fraction of the total binding energy of the cluster. Similar effects appear in other kinds of physical systems as well; mesic atoms behave in much the same way. The phase volumes of two otherwise equivalent stellar systems, each dominated by a tightly bound binary, favor exchange to incorporate the more massive star in the binary by a factor equal to the cube of the ratio of masses.

Type
Part I/Spherical Systems
Information
Symposium - International Astronomical Union , Volume 69: Dynamics of Stellar Systems , 1975 , pp. 95 - 97
Copyright
Copyright © Reidel 1975 

References

Aarseth, S. J.: 1971, Astrophys. Space Sci. 13, 324.CrossRefGoogle Scholar
Doede, John H.: 1964, Phys. Rev. 132, 1782.CrossRefGoogle Scholar
Miller, R. H.: 1973, Astrophys. J. 180, 759.CrossRefGoogle Scholar
Miller, R. H.: 1974, Advances in Chemical Physics 26, 107.Google Scholar