A Two-dimensional Computational Comparison of the Dynamic Interactions of Critical and Subcritical Mass Proto--Globular Cluster Clouds with the Protogalactic Background

Details A Two-dimensional Computational Comparison of the Dynamic Interactions of Critical and Subcritical Mass Proto--Globular Cluster Clouds with the Protogalactic Background A Two-dimensional Computational Comparison of the Dynamic Interactions of Critical and Subcritical Mass Proto--Globular Cluster Clouds with the Protogalactic Background

Apr 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997apj...479..792d&link_type=abstract

Astrophysical Journal v.479, p.792

Astronomy and Astrophysics

Astronomy

10

Galaxy: Globular Clusters: General, Hydrodynamics, Instabilities, Stars: Formation

Scientific paper

This paper presents a series of two-dimensional hydrodynamic simulations which examine the survival of proto--globular cluster clouds (PCCs) against hydrodynamic and gravitational instabilities. The simulations take a full accounting of the self-gravity of the PCCs by solving the Poisson equation in a self-consistent manner at each time step. Cooling effects are also included. 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 ~380 times that of the background, they begin to drop toward the galactic center and the background density increases. As they gain velocity Kelvin-Helmholtz (K-H) and Rayleigh-Taylor (R-T) instabilities form on the surface. The time constraints on PCC survival due to these instabilities and gravitational collapse are discussed in the context of collision-induced (Murray & Lin) and supernova-induced (Brown, Burkert, & Truran) globular cluster star formation scenarios.

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