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Session 17 - Molecular Clouds and Star Formation.
Oral session, Monday, June 10
Humanities 2650,
In this paper I present a series of two dimensional hydrodynamic simulations which examine the survival of proto globular cluster clouds (PCCs) between the time of formation and the formation of the currently observed stars. The simulations take a full accounting of the self-gravity by solving the Poisson equation in a self-consistent manner at each time step. Cooling effects are also included in all but one simulation. The PCCs begin at rest and in equilibrium with their own self-gravity and the pressure of the external medium. However, since their density is \sim 380 times that of the background they begin to drop toward the galactic center and increasing background density. As they gain velocity Kelvin - Helmholtz (K-H) and Rayleigh - Taylor (R-T) instabilities form on the surface. The R-T instabilities are only significant in simulations with cooling and are seeded by the collisions with cloudletts which condense from the gas sublimated from the PCC surface. The time constraints on PCC survival due to these instabilities and PCC collapse are discussed in the context of collision induced and supernova induced globular cluster star formation.
