Some relativistic features of non-rotating isothermal spheres - Motivation and numerical relativity

Details Some relativistic features of non-rotating isothermal spheres - Motivation and numerical relativity Some relativistic features of non-rotating isothermal spheres - Motivation and numerical relativity

Jan 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990ap%26ss.163..109s&link_type=abstract

Astrophysics and Space Science (ISSN 0004-640X), vol. 163, no. 1, Jan. 1990, p. 109-125.

Statistics

Computation

Isothermal Processes, Relativistic Theory, Rotating Spheres, Star Formation, Stellar Structure, Computational Astrophysics, Neutron Stars, Star Clusters, Stellar Mass

Scientific paper

The Tolman-Oppenheimer-Volkoff (TOV) equations of hydrostatic equilibrium are used to study the structure of high-density steady isothermal spheres. Analytic solutions to these TOV equations are given in the (xi, psi), (xi, U), (u, v) phase planes. The qualitative behaviors of the ratios of gas density to central density, pressure to central density, and the metric component are described for three representative general relativistic isothermal configurations, sigma = 0.1, 0.2, and 0.3. It is shown that the velocity of sound inside the configurations is always less than the velocity of light.

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