Statistics – Computation
Scientific paper
Oct 1989
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989apj...345..666g&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 345, Oct. 15, 1989, p. 666-673. Research supported by NSERC.
Statistics
Computation
24
Cooling Flows (Astrophysics), Galactic Clusters, Intergalactic Media, Computational Fluid Dynamics, Elliptical Galaxies, Gas Flow, Thermal Conductivity, Virgo Galactic Cluster
Scientific paper
The effect of thermal conduction on the evolution of cooling accretion flows is examined starting from the Chevalier (1987) similarity solution for an initially hydrostatic and isothermal gas in a singular isothermal potential. Conduction is found to slow the development of the cooling accretion flow. An initial cooling and subsonic settling phase, in which the core gas remains nearly isothermal, is increasingly prolonged as the thermal conduction parameter is increased. If conductive heating is sufficiently large, the subsonically settling gas appears to approach a steady state in which radiative cooling losses are balanced by conductive heating. Once the central temperature falls below the critical value for conductive stabilization, conductive heating of the core becomes less effective and a runaway thermal collapse follows. The duration of the thermal collapse of the core is roughly the initial central isobaric cooling time scale tau(iso). The results confirm that tau(iso) which is much shorter than a Hubble time does not guarantee that a cooling accretion flow has formed.
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