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A self-consistent field method for galactic dynamicsThe present study describes an algorithm for evolving collisionless stellar systems in order to investigate the evolution of systems with density profiles like the R exp 1/4 law, using only a few terms in the expansions. A good fit is obtained for a truncated isothermal distribution, which renders the method appropriate for galaxies with flat rotation curves. Calculations employing N of about 10 exp 6-7 are straightforward on existing supercomputers, making possible simulations having significantly smoother fields than with direct methods such as tree-codes. Orbits are found in a given static or time-dependent gravitational field; the potential, phi(r, t) is revised from the resultant density, rho(r, t). Possible scientific uses of this technique are discussed, including tidal perturbations of dwarf galaxies, the adiabatic growth of central masses in spheroidal galaxies, instabilities in realistic galaxy models, and secular processes in galactic evolution.
Document ID
19920041614
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Hernquist, Lars
(Lick Observatory Santa Cruz, CA, United States)
Ostriker, Jeremiah P.
(Princeton University Observatory, NJ, United States)
Date Acquired
August 15, 2013
Publication Date
February 20, 1992
Publication Information
Publication: Astrophysical Journal, Part 1
Volume: 386
ISSN: 0004-637X
Subject Category
Astrophysics
Accession Number
92A24238
Funding Number(s)
CONTRACT_GRANT: NSF AST-90-18526
CONTRACT_GRANT: NAGW-2422
CONTRACT_GRANT: NSF AST-90-06958
Distribution Limits
Public
Copyright
Other

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