On the quasihydrostatic flows of radiatively cooling self-gravitating gas clouds

Details On the quasihydrostatic flows of radiatively cooling self-gravitating gas clouds On the quasihydrostatic flows of radiatively cooling self-gravitating gas clouds

Mar 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995stin...9530729m&link_type=abstract

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Physics

Cooling, Lagrangian Function, Losses, Plasmas (Physics), Specific Heat, Collapse, Plasma Slabs

Scientific paper

Two model problems are considered, illustrating the dynamics of quasihydrostatic flows of radiatively cooling, optically thin self-gravitating gas clouds. In the first problem, spherically symmetric flows in an unmagnetized plasma are considered. For a power-law dependence of the radiative loss function on the temperature, a one-parameter family of self-similar solutions is found. The authors concentrate on a constant-mass cloud, one of the cases, when the self-similarity indices are uniquely selected. In this case, the self-similar flow problem can be formally reduced to the classical Lane-Emden equation and therefore solved analytically. The cloud is shown to undergo radiative condensation, if the gas specific heat ratio (gamma) greater than 4/3. The condensation proceeds either gradually, or in the form of (quasihydrostatic) collapse. For (gamma) less than 4/3, the cloud is shown to expand. The second problem addresses a magnetized plasma slab that undergoes quasihydrostatic radiative cooling and condensation. The problem is solved analytically, employing the Lagrangian mass coordinate.

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