Evolving, dynamical models for collapsed-core globular clusters - M15 and NGC 6624

Details Evolving, dynamical models for collapsed-core globular clusters - M15 and NGC 6624 Evolving, dynamical models for collapsed-core globular clusters - M15 and NGC 6624

Jun 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992apj...392...86g&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 392, no. 1, June 10, 1992, p. 86-98.

Astronomy and Astrophysics

Astronomy

64

Astronomical Models, Dynamic Models, Globular Clusters, Gravitational Collapse, Stellar Motions, Black Holes (Astronomy), Degenerate Matter, Fokker-Planck Equation, Pulsars, Stellar Mass, Velocity Distribution

Scientific paper

The stellar populations of the collapsed-core globular clusters M15 and NGC 6624 are investigated by fitting observed surface-brightness and projected velocity-dispersion profiles. The present evolving cluster models were generated by the direct Fokker-Planck method and incorporate realistic stellar mass spectra and energy input from binaries formed by three-body interactions. An evolved power-law mass function with nonluminous remnants of maximum mass 1.0-1.4 solar mass is adopted. M15 is found to be best fitted by postcollapse evolving models with a mass-function slope of x = 0.9 (where x = 1.35 corresponds to the Salpeter mass function) and a maximum remnant mass of 1.3 solar mass. Postcollapse core oscillations, driven by energy input from hard binaries, can produce sufficiently rapid core expansion to explain the resolution of the core of M15 by HST observations reported by Lauer et al. (1991).

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