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Spherical Stellar Systems: Structure and Evolution

Published online by Cambridge University Press:  04 August 2017

L. M. Ozernoy
Affiliation:
Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138
V. A. Volodin
Affiliation:
Lebedev Physical Institute, Moscow 117924, U.S.S.R.

Abstract

We analyze a class of spherical stellar systems with an isotropic, non-isothermal, one-particle distribution function which is truncated in energy ε as (ε b —ε)ν (ν > 0) near the energy of truncatingε b and is the Maxwell-Boltzmannian at |ε| ≫ |ε b |. the stellar systems which correspond to this distribution function appear to be isothermal in their central parts and polytropic in the external parts. Some qualitative results which follow from such a “polytropic-isothermal” distribution function (PIDF) are briefly discussed. A further extention of PIDF enables us to analyze in a new way the evolution of spherical stellar systems.

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Copyright
Copyright © Reidel 1987 

References

Cohn, H., 1980. Astrophys. J., 242, 765.CrossRefGoogle Scholar
King, I. R. 1966. Astron. J., 71, 64.CrossRefGoogle Scholar

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