Astronomy and Astrophysics – Astrophysics
Scientific paper
Dec 1980
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980azh....57.1287s&link_type=abstract
(Astronomicheskii Zhurnal, vol. 57, Nov.-Dec. 1980, p. 1287-1294.) Soviet Astronomy, vol. 24, Nov.-Dec. 1980, p. 741-745. Trans
Astronomy and Astrophysics
Astrophysics
1
Chemical Composition, Cosmology, Galactic Evolution, Gas Temperature, Gravitational Collapse, Interstellar Gas, Astrophysics, Electron Density (Concentration), Ionization, Molecular Gases, Shock Waves, Stellar Evolution, Thermochemistry
Scientific paper
The thermal evolution of a spherical gas cloud with a primordial chemical composition, contracting under the influence of gravity, is calculated. Initial densities and initial temperatures were varied in the range of 0.1-10/cu cm and 3-10 x 1000 K, respectively, in order to determine the class of initial conditions required to form a significant amount of H2 and H2(+) molecules and, as a consequence, cool the protogalactic gas to a low temperature (approximately equal to 100 K). The influence of radiation, produced by protoclusters of galaxies, on the amount of molecular hydrogen in the protogalactic material is examined. The destruction of H2 molecules by radiation is so efficient, that when z is not less than 2, the molecular hydrogen is able to cool the gas only when the initial density equals 10/cu cm. When the initial density is less than 10/cu cm and z is not less than 2, the gas contracts isothermally with the temperature approximately equal to 8000 K, and star formation is hindered. Under these conditions heavy elements are required to cool the gas to a temperature of 1000 K or lower.
Edelman M. A.
Shchekinov Yu A.
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