Gas cloud collisons in protogalaxies. I. Numerical simulations

Journal Article · Sun Aug 01 04:00:00 EDT 1982 · Astrophys. J.; (United States)

DOI:https://doi.org/10.1086/160152· OSTI ID:6806193

Struck-Marcell, C

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 H/sub 2/ formed in the dense, post-shock gas can, in some range of the collision parameters, cool the gas to a relatively low temperature (< or approx. =300 K). This temperature may be much lower than the precollision cloud temperature.

• Research Organization: Yale University Observatory
• OSTI ID: 6806193
• Journal Information: Astrophys. J.; (United States), Journal Name: Astrophys. J.; (United States) Vol. 259:1; ISSN ASJOA
• Country of Publication: United States
• Language: English

Related Subjects

640105* -- Astrophysics &amp; Cosmology-- Galaxies
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
CHEMICAL REACTIONS
COLLISIONS
COOLING
COSMIC GASES
FLUID MECHANICS
FLUIDS
GALAXIES
GASES
HEATING
HYDRODYNAMICS
IONIZATION
MATHEMATICAL MODELS
MATHEMATICS
MECHANICS
NUMERICAL ANALYSIS
RECOMBINATION
SHOCK WAVES