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Evolution of globular clusters in the Galaxy
Chernoff, David F.; Weinberg, Martin D.
AA(Cornell University, Ithaca, NY), AB(Cornell University, Ithaca, NY; Institute for Advanced Study, Princeton, NJ)
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 351, March 1, 1990, p. 121-156. Research supported by Sun Microsystems, Inc. and IBM Corp. (ApJ Homepage)
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NASA/STI Keywords:
Globular Clusters, Milky Way Galaxy, Stellar Evolution, Stellar Physics, Brightness Distribution, Fokker-Planck Equation, Many Body Problem, Mass To Light Ratios, Poisson Equation, Stellar Luminosity, Stellar Mass
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Globular cluster evolution is studied, modeling relaxation and energy exchange between the stars. A comprehensive survey is presented of Galactic globular cluster evolution until core collapse. Mass loss during the first five billion years is sufficiently strong to disrupt weakly bound clusters with a Salpeter initial mass function (IMF). The slope of the IMF is the critical parameter governing cluster survival during the mass-loss phase. Cluster which survive this initial phase then begin to collapse. Those with smaller mass and/or smaller Galactocentric orbital radii complete their core collapse by the present time. Two evolutionary endpoints are studied in detail: (1) the disruption of weakly bound clusters by mass loss due to stellar evolution, and (2) core collapse of multimass clusters. The state in which the multimass clusters exist today, if they have neither disrupted nor collapsed, is discussed. A number of observables based on stellar evolution calculations are presented.

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