Late core collapse in gravitating systems

Details Late core collapse in gravitating systems Late core collapse in gravitating systems

Oct 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979apj...233..694d&link_type=abstract

Astrophysical Journal, Part 1, vol. 233, Oct. 15, 1979, p. 694-703.

Astronomy and Astrophysics

Astrophysics

1

Astrophysics, Globular Clusters, Gravitational Collapse, Stellar Evolution, Astronomical Models, Cores, Energy Transfer, Fokker-Planck Equation, Stellar Mass, Time Dependence

Scientific paper

The late stages of the evolution of a star cluster are studied using a simplified two-region model. The primary interest is to determine the manner in which the central core collapses and to compare it with the simple homological evaporation model. Results indicate that self-interactions between core stars are the dominant evolutionary mechanism, leading to the evaporation of stars from the self-gravitating core. These stars do not escape from the entire cluster, but instead freeze out at intermediate radii because eventually the collapse causes the core radius to decrease below their orbital pericenters. It is found that the homological evaporation model gives a good description of the time-dependent behavior of the system. However, the rate of collapse may be different from that of the early stages, when the evaporating stars are escaping from the entire cluster or are accumulating in a far halo.

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