Physics – Fluid Dynamics
Scientific paper
Nov 2004
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004aps..dfd.jk020m&link_type=abstract
American Physical Society, 57th Annual Meeting of the Division of Fluid Dynamics, 21-23 November, 2004, Seattle, Washington, MEE
Physics
Fluid Dynamics
Scientific paper
During the epoch of large galaxy formation, thermal instability leads to the formation of a population of cool fragments embedded within a background of tenuous hot gas. The hot gas achieves near-hydrostatic equilibrium. Although the cool clouds are pressure confined by the hot gas, they fall into the galactic potential, and their motion is subject to drag from the hot gas. The release of gravitational energy due to the infall of the cool clouds is first converted into their kinetic energy, and is subsequently dissipated as heat. The cool clouds therefore represent a potentially significant energy source for the background hot gas, depending upon the ratio of thermal energy deposited within the clouds versus the hot gas. We have performed simulations to show that most of dissipated energy is deposited in the tenuous hot halo gas, providing a source of internal energy to replenish losses in the hot gas through bremsstrahlung emission and conduction into the cool clouds.
Lin Douglas
Murray Stephen S.
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