Post-collapse evolution of globular clusters

Details Post-collapse evolution of globular clusters Post-collapse evolution of globular clusters

Jul 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983mnras.204p..19s&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 204, July 1983, p. 19P-22P.

Mathematics

Probability

65

Binary Stars, Globular Clusters, Gravitational Collapse, Many Body Problem, Stellar Evolution, Astronomical Models, Celestial Mechanics, Density Distribution, Energy Transfer, Nonlinear Systems, Stellar Oscillations, Temperature Profiles, Thermal Expansion, Thermal Instability

Scientific paper

By means of a self-gravitating gaseous model it has been shown that a globular cluster core makes a non-linear oscillation with an amplitude as large as a factor of 106 in the central density. Core contraction is due to the gravothermal catastrophe. Switching from the contraction to expansion is performed by a small amount of energy input from binary stars. The expansion is driven also by a gravothermal instability but in the opposite direction. Since the oscillation is much slower in stages with lower densities, the probability is much higher of finding post-collapse globular clusters in states with the lower central densities than in the collapsed states with a high-density cusp.

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