Globule formation in a disturbed converging shock

Details Globule formation in a disturbed converging shock Globule formation in a disturbed converging shock

Aug 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991mnras.251..664k&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 251, Aug. 15, 1991, p. 664-669.

Astronomy and Astrophysics

Astronomy

12

Gas-Gas Interactions, Globular Clusters, Interstellar Gas, Molecular Clouds, Shock Waves, H Ii Regions, Hydrodynamics, Hydrogen Clouds, Star Formation

Scientific paper

This paper presents results of hydrodynamical simulations of a cylindrical gas cloud strongly pushed by a surrounding high-pressure gas. A perturbation on the cloud surface is introduced, and its evolution is numerically followed. A distorted shell of high-density shocked gas is formed from the cloud surface. The distortion of the shocked shell increases as the shell converges toward the center, and high-density gas clumps are formed behind the perturbed shock. The gas clumps gradually separate from the shell and eventually drift in the surrounding high-temperature region. For parent clouds with initial radius of 5-50 pc and density of 20-270/cu cm, gas clumps are formed in the order of 10 to the 6th yr. Their size and density are 0.1-3.0 pc and 100-10,000/cu cm, respectively, so their mass is several to several hundreds of solar masses, which is larger or close to the local Jeans mass. These physical properties of gas clumps are very similar to those of isolated dark globules, suggesting new mechanisms for the origin of isolated dark globules and stars.

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