**AAS 198th Meeting, June 2001**

*Session 65. Computational Astrophysics*

Display, Wednesday, June 6, 2001, 10:00am-7:00pm, Exhibit Hall
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## [65.02] Axisymmetric Self-Similar Equilibria of Self-Gravitating Isothermal Systems

*A. Umnov (Kurchatov Inst.), M. V. Medvedev (Harvard & CITA), R. Narayan (Harvard)*

Simple models of a self-gravitating gas are often used to
describe or model the structure of molecular clouds, in
studies of star formation, etc. Therefore, rigorous
analytical results are welcome. Here we study and classify
the structure of all possible axisymmetric self-similar
equilibrium configurations of self-gravitating, rotating,
isothermal systems. We show that there are two families: (1)
Cylindrically symmetric solutions in which the density
varies with cylindrical radius as R^{-2(n+1)}, with -1\le
n\le0. (2) Axially symmetric solutions in which the density
varies as f(\theta)/r^{2}, where r is the spherical radius
and \theta is the co-latitude. The singular isothermal
sphere is a special case of the latter class with
f(\theta)={\rm constant}. The axially symmetric
equilibrium configurations form a two-parameter family of
solutions and include equilibria which are asymmetric with
respect to the equatorial plane. We investigate whether the
asymmetric equilibria are force-free at the singular points
r=0, \infty, as well as their relevance to real systems.
For each hydrodynamic equilibrium, we determine the
phase-space distribution of the collisionless analog.

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