Statistics – Computation
Scientific paper
Aug 1985
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985mnras.215..499b&link_type=abstract
Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 215, Aug. 1, 1985, p. 499-507.
Statistics
Computation
6
Computational Astrophysics, Stellar Evolution, Stellar Mass, Stellar Systems, Density Distribution, Stellar Oscillations, Stellar Temperature
Scientific paper
Evolution of multi-mass stellar systems is followed by integrating numerically gas-model equations. A 10-component system in pre-collapse and two-component systems in post-collapse are studied. The most massive stars sediment towards the centre and approach a sharp, step-like density distribution. Starting from a state with equal velocity dispersions the evolved cluster does not approach global equipartition, although a high degree of equipartition of the kinetic energies develops in the central parts. Late-phase pre-collapse evolution of the most massive component occurs independently from the other components. Post-collapse evolution of the two-component system due to hardening of three-body binary stars can either show an ever expanding or an oscillating core, depending on the amount of energy released during high-density phases and the total mass of the more massive species. Oscillations are driven by the self-sustaining gravothermal expansion and contraction instabilities.
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