Astronomy and Astrophysics – Astronomy
Scientific paper
Dec 1994
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994pasj...46..567u&link_type=abstract
PASJ: Publications of the Astronomical Society of Japan (ISSN 0004-6264), vol. 46, no. 6, p. 567-574
Astronomy and Astrophysics
Astronomy
13
Astronomical Models, Black Holes (Astronomy), Cosmology, Dark Matter, Deposition, Galactic Evolution, Gas Pressure, Radiation Effects, Gravitational Effects, Hydrodynamics, Mathematical Models, Pressure Effects
Scientific paper
The spherically symmetric gas accretion regulated by external radiation drag is investigated under the steady-state approximation. As for the gravitational force, the dark-matter/point mass potentials as well as the self-gravity are considered. The radiation drag force is proportional to the velocity vector v as - beta v, where beta is a coefficient which is determined by the intensity of the radiation fields. We seek steady solutions under the assumption that beta is constant spatially and temporally. The analyses are separately made for a cold regime where the gas pressure is ignored and for a warm regime where the effects of pressure are included. In all of the cases considered, analytic steady solutions are found for spherical gas accretion with radiation drag. They include a modified solution for the Bondi accretion. Accretion via radiation drag may be a key process for the formation of condensed objects in the early universe shortly after cosmological recombination during which the radiation density of the Cosmic Background Radiation (CBR) is sufficiently high. If the universe is dominated by dark matter, in the early stage of the evolution of high-density peaks, the gas would accrete in the dark-matter potential. In the later stage and/or in the central region, the self-gravity becomes important compared to the dark-matter potentials. If the central dense core evolves into a black hole, in the last stage and/or in the very center, the gas would accrete in the point-mass potential exerted by the black hole. The obtained solutions are applicable for each phase.
Fukue Jun
Umemura Masayuki
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