Cooling of gas behind the explosive shocks and consequent star-formation in the central region of a disk galaxy.

Details Cooling of gas behind the explosive shocks and consequent star-formation in the central region of a disk galaxy. Cooling of gas behind the explosive shocks and consequent star-formation in the central region of a disk galaxy.

Aug 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991injpb..65..299k&link_type=abstract

Indian J. Phys., Part B, Vol. 65, No. 4, p. 299 - 311

Physics

Disk Galaxies: Star Formation, Disk Galaxies: Shock Waves

Scientific paper

Propagation of a shock produced by a nuclear explosion in a disk galaxy through a medium of constant density has been considered for different values of the initial Mach number. Cooling times have been computed under various shock conditions using a polytropic relation between the density and temperature within the cooling layer both in the presence and absence of a magnetic field. The relative amount of the shocked material which is likely to produce the molecular clouds has also been considered under different shock conditions. Calculations indicate that weaker shocks are probably more efficient for the formation of star than stronger shocks.

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