Radiatively-Cooling Self-Gravitating Gas
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**Session 53 -- Cluster Cooling Flows and Abundances**
*Display presentation, Thursday, January 13, 9:30-6:45, Salons I/II Room (Crystal Gateway)*

## [53.09] Radiatively-Cooling Self-Gravitating Gas

*P.N. Foster (DTM)*

We study radiatively cooling self-gravitating flows.
The early transitional stage of cooling flows, from
a static medium to a steady state inflow, as well as the
implications for galaxy formation, are considered
with this analysis.
We find a self-similar solution to describe this inflow, and
perform numerical modeling to test the breadth of initial
conditions which will follow the analytical solutions.
The self-similar solution incorporates a power law cooling term
which is
$\propto \rho^2 T^\lambda$;
if $\lambda<1$ the central temperature increases with time.
The paradoxical result of the temperature of cooling gas
increasing with time is due to strong gravitational compression.
This is confirmed with numerical simulations for $\lambda \leq -0.5$
that have moderately long central cooling times. Shorter cooling
times lead to a central thermal runaway. For simulations with
$\lambda > -0.5$, the center always cooled catastrophically
and never followed the self-similar solution.
We consider the observational consequences of the large luminosities
calculated from these models.

**Thursday
program listing**