Other
Scientific paper
Mar 1986
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986apj...302...81s&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 302, March 1, 1986, p. 81-94.
Other
25
Interstellar Matter, Molecular Clouds, Quasars, Seyfert Galaxies, Spectral Line Width, Stellar Winds, Emission Spectra, Galactic Nuclei, Plasma-Particle Interactions, Shock Fronts, Wind Velocity
Scientific paper
In this paper we investigate the interaction between a "quasar wind," as proposed by Weymann et al. (1982) and interstellar clouds in a Seyfert galaxy. The propagation of the wind into the low-density gas component of the interstellar medium (ISM) was studied in Schiano (1985), and the wind velocity field determined there is used to determine the physical structure and motion of interstellar clouds. The cloud component of the ISM of a Seyfert galaxy (cloud sizes, content, distribution and so on) is modeled by assuming that these galaxies are similar to the Milky Way and other nearby "nonactive" galaxies. The wind-cloud interaction is studied in a qualitative manner using the results of published hydrodynamic calculations for the interaction of shock fronts with interstellar clouds and the radiation transfer calculations appropriate for narrow emission line clouds. The motion of the clouds is then determined, using the effective wind velocity field described in Schiano (1985) and a model gravitational field. The results show that the initially rarefied clouds (n < 10-2 cm-2) are thermally unstable and rapidly driven from the inner regions (a few kiloparsecs) of an average Seyfert galaxy. The densest clouds (molecular clouds) are thermally stable but are heated to ˜ 104 K throughout most of their volumes. Clouds with masses less than 103 Msun can be accelerated by wind ram pressure to velocities in excess of the galactic escape velocity. Given the physical conditions and velocities of these clouds, it is proposed that the narrow emission line regions (NELRs) of Seyfert galaxies are the result of the interaction of active galactic nuclei ionizing photons and a thermal wind on dense, massive interstellar clouds. Arguments are presented to show that NELR clouds must be massive and unable to be accelerated to observed NELR velocities by photon momentum alone. A discussion of observable consequences of the wind is also presented.
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