Gas cloud collisions in protogalaxies. I - Numerical simulations

Details Gas cloud collisions in protogalaxies. I - Numerical simulations Gas cloud collisions in protogalaxies. I - Numerical simulations

Aug 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982apj...259..116s&link_type=abstract

Astrophysical Journal, Part 1, vol. 259, Aug. 1, 1982, p. 116-126.

Physics

25

Astronomical Models, Cloud Physics, Collision Parameters, Computerized Simulation, Galactic Evolution, Hydrogen Clouds, Gas Temperature, Hydrodynamic Equations, Interstellar Gas, Particle Interactions, Stellar Evolution, Time Dependence

Scientific paper

A series of time-dependent, numerical hydrodynamical simulations of high-velocity atomic gas cloud collisions in protogalaxies is presented. The protogalactic gas is assumed to be essentially metal-free. The processes of heating, cooling, ionization, recombination, molecule formation and destruction are included in the simulations. The outcome of a cloud collision is found to depend sensitively on the detailed microphysics. In particular, a small amount of H2 formed in the dense, post-shock gas can, in some range of the collision parameters, cool the gas to a relatively low temperature (lower than about 300 K). This temperature may be much lower than the precollision cloud temperature, and thus the cold gas may be very susceptible to star formation.

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