Observational evidence for the radiative acceleration of broad-line clouds in Seyfert 1 galaxies and quasars

Details Observational evidence for the radiative acceleration of broad-line clouds in Seyfert 1 galaxies and quasars Observational evidence for the radiative acceleration of broad-line clouds in Seyfert 1 galaxies and quasars

Apr 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985apj...291..112g&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 291, April 1, 1985, p. 112-116. Research supported by Cambridge University,

Astronomy and Astrophysics

Astrophysics

45

H Beta Line, Interstellar Gas, Line Spectra, Quasars, Seyfert Galaxies, Spectral Line Width, Astronomical Models, Balmer Series, Collision Rates, Emission Spectra, Ionized Gases, Optical Thickness, Radiative Transfer

Scientific paper

While the relative strength of the broad H-beta emission line in Seyfert 1 galaxies depends on the width of the lines, so that it is very weak for objects with narrow lines, the equivalent width of Fe II 4570 A is independent of velocity width. Calculations indicate that the decrease in equivalent width of H-beta is due to either slightly higher densities or slightly larger optical depths in the partially ionized zones of the narrow-line Seyfert 1 galaxy broad-line clouds. The correlation of H-beta emissivity with cloud velocity furnishes strong support for the radiative acceleration models developed by Mathews and Blumenthal (1977). It is suggested that the cause of object-to-object variations is the pressure of the hot, confining intercloud medium, whose pressure differences are also the cause of the difference in broad line properties between broad line radio galaxies and radio-quiet objects.

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