Thermal and Dynamical Evolution of Intergalactic Clouds

Details Thermal and Dynamical Evolution of Intergalactic Clouds Thermal and Dynamical Evolution of Intergalactic Clouds

Jul 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984pthph..72...47u&link_type=abstract

Progress of Theoretical Physics, Vol. 72, No. 1, pp. 47-62

Physics

42

Cosmology: Theory, Galaxies: Formation, Hydrodynamics, Intergalactic Medium

Scientific paper

Assuming that the intergalactic clouds with the mass 10(7 ~) 10(13) M_sun were born at the epoch z=5 ~ 10, their thermal and dynamical evolution is numerically explored. The clouds with tha mass greater than 10(9M_sun) had collapsed by the present epoch, and their evolution weakly depends upon the mass. We may assign these collapsed clouds to quasars and galaxies. The clouds with the mass smaller than 10(9M_sun) can keep expansion, and their evolution is characterized as pressure confined clouds. Physical quantities of these expanding clouds well correspond to the Lyman alpha absorbers of QSO lights. Some relevant problems to the present calculations such as the formation of a massive halo and the mass spectrum of intergalactic clouds are discussed briefly.

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