Shock propagation in a turbulent cloud

Details Shock propagation in a turbulent cloud Shock propagation in a turbulent cloud

Apr 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993apj...406..512k&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 406, no. 2, p. 512-519.

Statistics

Computation

11

Hydrodynamic Equations, Molecular Clouds, Shock Wave Interaction, Shock Wave Propagation, Turbulence Effects, Computational Astrophysics, H Ii Regions, Velocity Distribution

Scientific paper

A 2D hydrodynamical simulation is used to investigate the effect of internal turbulence of molecular clouds on the shock waves propagating in the clouds. A model of a turbulent molecular cloud dynamically interacting with the surrounding H II region, which strongly compresses the cloud from the surface, is considered. A shock wave is generated from the cloud surface and propagates into the cloud, where a supersonic random velocity field and large density fluctuation are present. The turbulence strongly affects the propagation of the shock wave to cause a very complex and fragmentary structure in the shocked gas. Behind the distorted shock, many high-density gas clumps are formed. It is argued that the interaction of the internal turbulence of a molecular cloud and a shock wave will play an important role in the formation of high-density gas clumps and stars when a molecular cloud interacts with an expanding H II region.

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