Other
Scientific paper
Aug 1987
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987apj...319..772l&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 319, Aug. 15, 1987, p. 772-800.
Other
31
Binary Stars, Globular Clusters, Main Sequence Stars, Stellar Evolution, Stellar Models, White Dwarf Stars, Fokker-Planck Equation, Gravitational Collapse, Neutron Stars, Stellar Mass, Three Body Problem
Scientific paper
Numerical studies of the dynamical evolution of globular clusters using an orbit-averaged isotropic Fokker-Planck code, including binary formation and their interactions with others, are presented. Two different initial stellar mass categories are assumed: main-sequence stars having individual masses mMS and degenerate stars (either white dwarfs or neutron stars) having individual masses mD such that mD/mMS> 1. Very hard binaries composed of degenerate-normal pairs are allowed to form via the tidal capture process and moderately hard degenerate-degenerate binaries are allowed to form via the three-body process. If the initial degenerate population is sufficiently large, the three-body binaries among degenerate stars eventually provide enough energy to stop the collapse and cause reexpansion. On the other hand, the degenerate-normal pair of tidally captured binaries are a relatively important energy source if the initial population of degenerate stars is small.
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