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Adiabatic invariants in stellar dynamics, 3: Application to globular cluster evolutionThe previous two companion papers demonstrate that slowly varying perturbations may not result in adiabatic cutoffs and provide a formalism for computing the long-term effects of time-dependent perturbations on stellar systems. Here, the theory is implemented in a Fokker-Planck code and a suite of runs illustrating the effects of shock heating on globular cluster evolution are described. Shock heating alone results in considerable mass loss for clusters with R(sub g) less than or approximately 8 kpc: a concentration c = 1.5 cluster with R(sub g) kpc loses up to 95% of its initial mass in 15 Gyr. Only those with concentration c greater than or approximately 1.3 survive disk shocks inside of this radius. Other effects, such as mass loss by stellar evolution, will decrease this survival bound. Loss of the initial halo together with mass segregation leads to mass spectral indices, x, which may be considerably larger than their initial values.
Document ID
19950032394
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Weinberg, Martin D.
(Univ. of Massachusetts, Amherst, MA United States)
Date Acquired
August 16, 2013
Publication Date
October 1, 1994
Publication Information
Publication: The Astronomical Journal
Volume: 108
Issue: 4
ISSN: 0004-6256
Subject Category
Astrophysics
Funding Number(s)
CONTRACT_GRANT: NSF PHY-89-04035
CONTRACT_GRANT: NAGW-2224
Distribution Limits
Public
Copyright
Other
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