Computer Science – Numerical Analysis
Scientific paper
Jan 1984
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984mnras.206..179h&link_type=abstract
Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 206, Jan. 1, 1984, p. 179-195.
Computer Science
Numerical Analysis
56
Astronomical Models, Globular Clusters, Gravitational Collapse, Numerical Analysis, Stellar Evolution, Stellar Systems, Binary Stars, Black Holes (Astronomy), Gas Density, Monte Carlo Method, Stellar Luminosity, Stellar Temperature, Time Dependence
Scientific paper
The evolution of an enclosed, spherical, stellar system is studied numerically. The system is modelled as a perfect gas with a thermal conductivity designed to resemble two-body relaxation and a source of energy modelling some of the effects of binary stars. The collapse of the core of the system is almost unaffected by the energy source until very high central densities are reached. Thereafter an isothermal region, with decreasing temperature, gradually extends through the cluster. Simple theoretical considerations yield results on the time-dependence of the central temperature, density and luminosity, in agreement with the numerical data. The theory is sufficiently general to be applied to problems with different types of energy source, and its predictions are in fair agreement with the published results of Monte Carlo simulations of clusters containing a black hole.
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