Volume 607, November 2017
|Number of page(s)||7|
|Published online||20 November 2017|
Interaction of the accretion flows in corona and disk near the black hole in active galactic nuclei
1 Max-Planck-Institut für Astrophysik, Karl- Schwarzschildstr. 1, 85740 Garching, Germany
2 Key Laboratory of Space Astronomy and Technology, National Astronomical Observatories, Chinese Academy of Sciences, 100012 Beijing, PR China
3 School of Astronomy and Space Science, University of Chinese Academy of Sciences, 19A Yuquan Road, 100049 Beijing, PR China
Received: 4 May 2017
Accepted: 29 August 2017
Context. Accretion flows toward black holes can be of a quite different nature, described as an optically thick cool gas flow in a disk for high accretion rates or as a hot coronal optically thin gas flow for low accretion rates, possibly affected by outflowing gas.
Aims. The detection of broad iron emission lines in active galactic nuclei (AGN) indicates the coexistence of corona and disk. The appearance and relative strength of such flows essentially depends on their interaction. Liu et al. suggested that condensation of gas from the corona to the disk allows to understand accretion flows of comparable strength of emission. Matter inflow due to gravitational capture of gas is important for the condensation process. We discuss observational features predicted by the model.
Methods. Data from simultaneous observations of AGN with Swift’s X-ray and UV-optical telescopes are compared with the theoretical predictions.
Results. The frequent detection of broad iron Kα emission lines and the dependence of the emitted spectra on the Eddington ratio, described by the values of the photon index Γ and the two-point spectral index αox are in approximate agreement with the predictions of the condensation model; the latter, however, with a large scatter. The model further yields a coronal emission concentrated in a narrow inner region as is also deduced from the analysis of emissivity profiles.
Conclusions. The accretion flows in bright AGN could be described by the accretion of stellar wind or interstellar medium and its condensation into a thin disk.
Key words: accretion, accretion disks / X-rays: binaries / X-rays: galaxies / galaxies: Seyfert / quasars: individual: Mrk 335
© ESO, 2017
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