Astronomy and Astrophysics – Astronomy
Scientific paper
Oct 1984
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984mnras.210..763l&link_type=abstract
Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 210, Oct. 15, 1984, p. 763-777.
Astronomy and Astrophysics
Astronomy
28
Astronomical Models, Black Holes (Astronomy), Globular Clusters, Density Distribution, Interstellar Magnetic Fields, Main Sequence Stars, Spatial Distribution, Stellar Luminosity, Stellar Mass Ejection, X Ray Sources
Scientific paper
If a globular cluster contains remnants much more massive than the visible stars, these remnants will dominate the cluster core, and will rapidly attain a nearly singular density distribution. Simple two-component models show that the observed light profiles and velocity dispersions of typical globular cluster cores are reproduced if the density of heavy remnants varies as r-2.5 at small radii, and if a representative mass for the heavy remnants is ≡2.5 M_sun;. The cusped light profile of M15 can be explained with a somewhat smaller representative mass of ≡1.7 M_sun; for the heavy remnants. A possible, but not unique, set of assumptions that can account for the remnant properties in a typical case is that the initial mass function is the same as that of the solar neighbourhood, and that the massive stars leave remnants whose mass is ≡15 per cent of the initial stellar mass. The extremes of small and large fractional content of heavy remnants are represented by 47 Tuc and ω Cen.
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