Kinetics of H2 formation in the primordial gas

Details Kinetics of H2 formation in the primordial gas Kinetics of H2 formation in the primordial gas

Feb 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984azh....61...24i&link_type=abstract

(Astronomicheskii Zhurnal, vol. 61, Jan.-Feb. 1984, p. 24-34) Soviet Astronomy (ISSN 0038-5301), vol. 28, Jan.-Feb. 1984, p. 15-

Astronomy and Astrophysics

Astronomy

2

Big Bang Cosmology, Galactic Evolution, Hydrogen Clouds, Interstellar Chemistry, Molecular Clouds, Abundance, Astronomical Models, H Lines, Lyman Alpha Radiation, Protostars, Reaction Kinetics

Scientific paper

Calculations are performed to determine the kinetics of molecular hydrogen formation in rarefied (about 0.1/cu cm), low-temperature (T not more than 10,000 K) primordial matter. Since the chemical reactions will not proceed in equilibrium, H2 will form efficiently, reaching a relative number density of about 0.001, enough to promote rapid cooling of the medium below 1000 K. The strongest H2 line emitted by a cosmological pancake during the H2 formation era will be the j = 2-0 rotational line, redshifted (for z = 3-5) to wavelengths of about 100-150 microns. If this line, whose flux density might well reach 1 Jy, should be detected, one might be able to ascertain the epoch and structure of the universe at the stage when galaxies and first-generation stars were born.

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