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Equilibrium stellar systems with spindle singularitiesEquilibrium sequences of axisymmetric Newtonian clusters that tend toward singular states are constructed. The distribution functions are chosen to be of the form f = f(E, Jz). The numerical method then determines the density and gravitational potential self-consistently to satisfy Poisson's equation. For the prolate models, spindle singularities arise from the depletion of angular momentum near the symmetry axis. While the resulting density enhancement is confined to the region near the axis, the influence of the spindle extends much further out through its tidal gravitational field. Centrally condensed prolate clusters may contain strong-field regions even though the spindle mass is small and the mean cluster eccentricity is not extreme. While the calculations performed here are entirely Newtonian, the issue of singularities is an important topic in general relativity. Equilibrium solutions for relativistic star clusters can provide a testing ground for exploring this issue. The methods used in this paper for building nonspherical clusters can be extended to relativistic systems.
Document ID
19920050384
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Shapiro, Stuart L.
(NASA Headquarters Washington, DC United States)
Teukolsky, Saul A.
(Cornell University Ithaca, NY, United States)
Date Acquired
August 15, 2013
Publication Date
April 1, 1992
Publication Information
Publication: Astrophysical Journal, Part 1
Volume: 388
ISSN: 0004-637X
Subject Category
Astrophysics
Accession Number
92A33008
Funding Number(s)
CONTRACT_GRANT: NSF PHY-90-07834
CONTRACT_GRANT: NSF AST-90-15451
CONTRACT_GRANT: NAGW-2364
Distribution Limits
Public
Copyright
Other

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