A theory of core collapse in clusters

Details A theory of core collapse in clusters A theory of core collapse in clusters

Aug 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979mnras.188..525h&link_type=abstract

Astronomy and Astrophysics, vol. 76, no. 3, July 1979, p. 525-554.

Astronomy and Astrophysics

Astrophysics

9

Binary Stars, Gravitational Collapse, Star Clusters, Star Distribution, Stellar Mass Ejection, Boundary Value Problems, Cores, Differential Equations, Mathematical Models, Maxwell-Boltzmann Density Function, Monte Carlo Method, Three Body Problem

Scientific paper

A new theory of core collapse in star clusters is based on the idea that only the distribution of stars moving on radial orbits is important. Self-similar solutions for the evolution of this distribution are found for different values of the energy of escape. As the energy increases, deviations from a Maxwellian distribution become relatively smaller, and the time-scale for core collapse increases relative to the central relaxation time. Comparison with the results of Monte Carlo models indicates a substantial measure of agreement, with one significant discrepancy. It is predicted that core collapse will be accompanied by a decrease in the central velocity dispersion if the escape energy is small enough. Further calculations indicate that the presence of a sufficient proportion of suitable hard binaries may arrest the collapse process.

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