Physics
Scientific paper
Jun 1975
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975apj...198..517b&link_type=abstract
Astrophysical Journal, vol. 198, June 15, 1975, pt. 1, p. 517-526. Research supported by the University of California
Physics
151
Emission Spectra, Line Spectra, Nebulae, Quasars, Seyfert Galaxies, Astronomical Spectroscopy, Cloud Physics, Cosmic Gases, Galactic Radiation, Interstellar Matter, Ultraviolet Radiation
Scientific paper
A model is analyzed in which the observed emission-line spectra of QSOs and Seyfert galaxies are due to a gas in the form of small clouds which can be accelerated to high velocities by UV radiation from a small central source and can be contained to very high densities by a high-pressure intercloud medium. It is shown that the outward motion of the cloud system generates a logarithmic emission-line profile for recombination lines which is independent of the mass distribution of the clouds, the change in gas temperature and density in the clouds, and the initial location of the cloud-forming region. The logarithmic profile is shown to agree very well with recently observed profiles for PSK 1217+02, PKS 2135-14, and 3C 273, except in the cores of the lines and occasionally in the far wings. It is shown how the basic logarithmic line profile is influenced by drag, gravity, chemical composition, dust, and other effects.
Blumenthal George R.
Mathews William G.
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