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Heat conduction in cooling flowsIt has been suggested that electron conduction may significantly reduce the accretion rate (and star foramtion rate) for cooling flows in clusters of galaxies. A numerical hydrodynamics code was used to investigate the time behavior of cooling flows with conduction. The usual conduction coefficient is modified by an efficiency factor, mu, to realize the effects of tangled magnetic field lines. Two classes of models are considered, one where mu is independent of position and time, and one where inflow stretches the field lines and changes mu. In both cases, there is only a narrow range of initial conditions for mu in which the cluster accretion rate is reduced while a significant temperature gradient occurs. In the first case, no steady solution exists in which both conditions are met. In the second case, steady state solutions occur in which both conditions are met, but only for a narrow range of initial values where mu = 0.001.
Document ID
19880044684
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Bregman, Joel N.
(National Radio Astronomy Observatory Charlottesville, VA, United States)
David, L. P.
(Virginia, University Charlottesville, United States)
Date Acquired
August 13, 2013
Publication Date
March 15, 1988
Publication Information
Publication: Astrophysical Journal, Part 1
Volume: 326
ISSN: 0004-637X
Subject Category
Astrophysics
Accession Number
88A31911
Funding Number(s)
CONTRACT_GRANT: NAGW-764
Distribution Limits
Public
Copyright
Other

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