Other
Scientific paper
Jul 1986
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986ap%26ss.124..295m&link_type=abstract
Astrophysics and Space Science (ISSN 0004-640X), vol. 124, no. 2, July 1986, p. 295-303.
Other
Cosmic Gases, Equations Of State, Gravitational Fields, Molecular Clouds, Stellar Gravitation, Density Distribution, Homology, Isothermal Processes, Polytropic Processes, Stellar Structure, Thermodynamic Properties
Scientific paper
It is shown that because of self-gravitational interaction, a cosmic gas which is perfect otherwise is destined to behave like an imperfect gas. It is found that for a cosmic gas in hydrostatic equilibrium the only mode of free expansion (or contraction) is by a homologous evolution. This theorem enables one to construct the equation of state in terms of the local thermodynamical parameters of the inhomogeneous medium in such a way that it is consistent with the boundary conditions at the center and at the natural boundary of the system. This method can be extended even when there is a temperature gradient in the system. This analysis predicts that the density profile should be the same at least for all nondegenerate Newtonian stars having the same temperature profile and which can be considered to be in hydrostatic equilibrium. The density profile will be that of a polytrope of index n = 3, modulated by a temperature profile.
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