Astronomy and Astrophysics – Astronomy
Scientific paper
Dec 1982
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982mnras.201..833n&link_type=abstract
Monthly Notices of the Royal Astronomical Society, vol. 201, Dec. 1982, p. 833-847. Research supported by the Science and Engin
Astronomy and Astrophysics
Astronomy
92
Astronomical Models, Gas Dynamics, Interstellar Gas, Shock Wave Interaction, Compression Waves, Finite Difference Theory, Gas Density, Gas Pressure, Gravitational Collapse, Taylor Instability
Scientific paper
Four distinct system evolution stages are established by a study of the impact of a strong interstellar shock with a high density gas cloud, using two different numerical techniques to solve the model equations. The formation of gravitationally unstable regions will be enhanced by the onset of Rayleigh-Taylor instabilities at the surface of the cloud, which develop because of the acceleration of the high density material of the gas cloud by the comparatively low density shocked interstellar gas. If the cloud survives the initial shock compression stage, it begins to expand. The complex post-shock flow field sets up a strong fluid rotation at the rear of the cloud, and the fast ambient interstellar gas pushes the cloud toward this rotating region to cause a secondary compression of the cloud. The gas reacts by expanding, aided by the rotating fluid region which whirls matter off the back of the gas cloud. The combined action of expansion and fluid rotation results in the eventual destruction of the cloud.
Falle Sam A. E. G.
Gaskell P. H.
Nittmann J.
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