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Article overview
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X-ray emitting-absorbing media in Seyfert 1 galaxies | M. Mouchet
; A. Abrassart
; D. Porquet
; A.-M. Dumont
; S. Collin
; | Date: |
13 Mar 2000 | Subject: | astro-ph | Affiliation: | DAEC, Observatoire de Paris-Meudon, Meudon, F), A. Abrassart (DAEC, Observatoire de Paris-Meudon), D. Porquet (SAp, CEA Saclay, F), A.-M. Dumont (DAEC, Observatoire de Paris-Meudon), S. Collin (DAEC, Observatoire de Paris-Meudon | Abstract: | Seyfert galaxies have been shown to exhibit a large variety of features in their X-ray spectra from which the environment of the central engine can be deduced. We focus on the two following aspects: the Warm Absorber, mainly responsible of the soft X-ray properties, and the reprocessing/reflecting plasma medium at the origin of the iron Kalpha fluorescent line. The physical parameters and the location of the so-called Warm Absorber (WA), a photoionized medium along the line of sight to the nuclear region, are more strongly constrained by optical coronal lines than by the oxygen edges observed in the soft X-rays and produced by the WA. The photoionization models also predict the intensities of the X-ray emission lines which are going to be detected with the new generation of X-ray satellites. An alternative model to the relativistic accretion disc is proposed to explain the profile of the X-ray iron Kalpha line observed in the Seyfert 1. This line can be formed in the framework of a quasi-spherical accretion of optically thick clouds. An optically thick photoionization code coupled with a Monte-Carlo code has been developed to compute the entire spectrum from the IR to the hard X-rays for a close geometry with a large covering factor. The multiple Compton reflections allow to reproduce the redshifted broad iron line as detected in several Seyfert 1 galaxies and in MCG-6-30-15. | Source: | arXiv, astro-ph/0003168 | Services: | Forum | Review | PDF | Favorites |
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