Reference : Eclipsing the innermost accretion disc regions in AGN
Scientific journals : Article
Physical, chemical, mathematical & earth Sciences : Space science, astronomy & astrophysics
http://hdl.handle.net/2268/231169
Eclipsing the innermost accretion disc regions in AGN
English
Sanfrutos, M. [Centro de Astrobiología (CSIC-INTA), Dep. de Astrofísica; ESAC, PO Box 78, Villanueva de la Cañada, E-28691 Madrid, Spain]
Miniutti, G. [Centro de Astrobiología (CSIC-INTA), Dep. de Astrofísica; ESAC, PO Box 78, Villanueva de la Cañada, E-28691 Madrid, Spain]
Dovčiak, M. [Astronomical Institute, Academy of Sciences, Boční II, CZ-14131 Prague, Czech Republic]
Agis-Gonzalez, Beatriz mailto [Centro de Astrobiología (CSIC-INTA), Dep. de Astrofísica, ESAC, PO Box 78, Villanueva de la Cañada, E-28691 Madrid, Spain > > > >]
1-May-2016
Astronomische Nachrichten
John Wiley & Sons
337
546
Yes (verified by ORBi)
International
00046337
15213994
United Kingdom
[en] accretion ; accretion disks ; black hole physics ; galaxies: active ; galaxies: nuclei ; relativistic effects ; X-rays: galaxies
[en] Variable X-ray absorption has been observed in active galactic nuclei (AGN) on several time scales. Observations allow us to identify the absorber with clouds associated either with the clumpy torus (parsec scales, long timescales) or with the broad line region (BLR) (short timescales). In the latter, the cloud size has been estimated to be of the order of few gravitational radii from the observed absorption variability. Such small cloud sizes are comparable to the X-ray emitting regions so that a detailed modeling of occultation events in AGN has the potential of enabling us to infer accurately the geometry of the system. We have developed a relativistic X-ray spectral model for occultation events and we present here theoretical predictions on the different observables that can be inferred by studying X-ray eclipses in simulated XMM-Newton data. These include the size of the X-ray emitting regions as well as more fundamental parameters such as the black hole spin and the system inclination. We find that absorption varies as a function of the energy range and that its maximum takes place when the approaching part of the accretion disc is covered. Therefore we study the hard-to-soft (H / S) ratio light curves produced during an eclipse and use them to characterise the properties of the inner accretion disc in a new model-independent way.
http://hdl.handle.net/2268/231169
10.1002/asna.201612345
http://adsabs.harvard.edu/abs/2016AN....337..546S

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