Cooling of primordial matter by molecular hydrogen

Details Cooling of primordial matter by molecular hydrogen Cooling of primordial matter by molecular hydrogen

Jun 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978sva....22..279k&link_type=abstract

(Astronomicheskii Zhurnal, vol. 55, May-June 1978, p. 487-489.) Soviet Astronomy, vol. 22, May-June 1978, p. 279, 280. Translat

Physics

1

Cloud Physics, Cooling, Cosmology, Hydrogen, Interstellar Gas, Molecular Gases, Gas Density, High Temperature Gases, Hydrogen Ions, Molecular Collisions, Nonequilibrium Conditions, Stellar Evolution

Scientific paper

The molecular hydrogen cooling function at temperatures of about 6000 to 10,000 K is computed, taking into account the nonequilibrium population of the rotational and vibrational levels at hydrogen densities of 1 to 1000 per cu cm. The results show that nonequilibrium effects caused by the difference between the (collisional) excitation mechanism and the (mainly radiative) deactivation mechanism under conditions where the kinetic temperature is much higher than the radiation temperature have a substantial influence on the molecular hydrogen cooling function. It is concluded that vibrational excitation of H2 contributes the most to energy removal and can therefore play an important part in the formation of the first generation of stars from matter of primordial chemical composition.

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