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Prog. Theor. Phys. Vol. 42 No. 3 (1969) pp. 523-543

[ Full Text PDF : FREE ACCESS (1424K) ]

Formation of Protogalaxies and Molecular Processes in Hydrogen Gas

Toshiaki Hirasawa

Department of Physics, Rikkyo University, Tokyo

(Received April 7, 1969)

Abstract:

As one stage of galaxy formation we study the gravitational contraction of a cold gas due to the radiative cooling by hydrogen molecules. Assuming that the gas consists mainly of hydrogen atoms, we consider all possible atomic and molecular processes in the gas and find that H2 molecules are formed most efficiently by way of H- formation: H+e- →H-+hν and H-+H →H2+e-. The contraction of a gas cloud is studied in the wide range of initial conditions and it is found that sufficient amounts of H2 are formed in the gas cloud so that it can evolve into a protogalaxy provided that the radiation temperature is less than 300°K. We also examine the effect of He and D on the cooling and find that their effect is negligible.


URL : http://ptp.ipap.jp/link?PTP/42/523/
DOI : 10.1143/PTP.42.523

[ Full Text PDF : FREE ACCESS (1424K) ] Citation:

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Citing Article(s) :

  1. Progress of Theoretical Physics Vol. 42 No. 2 (1969) pp. 219-233 :
    Cooling of Pre-Galactic Gas Clouds by Hydrogen Molecule
    Takuya Matsuda, Humitaka Satō and Hidenori Takeda
  2. Progress of Theoretical Physics Vol. 46 No. 2 (1971) pp. 416-432 :
    Dissipation of Primordial Turbulence and Thermal History of the Universe
    Takuya Matsuda, Humitaka Sato and Hidenori Takeda
  3. Progress of Theoretical Physics Vol. 55 No. 2 (1976) pp. 337-339 :
    Radiative Attachment of Electrons with Some Alkali Atoms
    Suresh Chandra and Udit Narain
  4. Progress of Theoretical Physics Vol. 77 No. 5 (1987) pp. 1152-1162 :
    Formation of the First Systems in the Wakes of Moving Cosmic Strings
    Tetsuya Hara and Shigeru Miyoshi
  5. Progress of Theoretical Physics Vol. 78 No. 5 (1987) pp. 1081-1098 :
    Flare-Up of the Universe after z ≃102 for Cosmic String Model
    Tetsuya Hara and Shigeru Miyoshi

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