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Heat conduction in cooling flows
Bregman, Joel N.; David, L. P.
AA(National Radio Astronomy Observatory, Charlottesville, VA), AB(Virginia, University, Charlottesville)
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 326, March 15, 1988, p. 639-644. (ApJ Homepage)
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NASA/STI Keywords:
Conductive Heat Transfer, Cooling, Galactic Clusters, Intergalactic Media, Electron Energy, Heat Flux, Interstellar Magnetic Fields, Star Formation Rate
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It 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.

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