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Date and Time of the Query: 2019-06-16 T06:11:35 PDT
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For refcode 1989ApJ...343..678K:
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1989ApJ...343..678K THE ORIGIN OF CORONAL LINES IN SEYFERT GALAXIES K. T. KORISTA AND G. J. FERLAND Ohio State University Received 1988 December 9; accepted 1989 January 24 ABSTRACT In this paper we examine the possibility that the coronal line region in Seyfert galaxies may be the result of an interstellar medium (ISM) exposed to, and subsequently photoionized by, a "bare" Seyfert nucleus. We show that a "generic" AGN continuum illuminating the warm-phase (N_e_ ~ 1 cm^-3^) of the ISM of a spiral galaxy can produce the observed emission. In this picture the same UV-radiation cone that is responsible for the high-excitation extended narrow-line emission clouds observed out to 1-2 kpc or farther from the nuclei of some Seyfert galaxies also produces the coronal lines. Soft X-rays originating in the nucleus are Compton- scattered off the ISM, thus producing extended soft X-ray emission, as observed in NGC 4151. The results of our calculations show a basic insensitivity to the ISM density, which explains why similar coronal line spectra are found in many Seyfert galaxies of varying physical environments. Subject headings: galaxies: interstellar matter - galaxies: Seyfert - radiation mechanisms
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