Modeling the X-ray spectra of magnetic flares in Active Galactic Nuclei

Details Modeling the X-ray spectra of magnetic flares in Active Galactic Nuclei Modeling the X-ray spectra of magnetic flares in Active Galactic Nuclei

Dec 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005sf2a.conf..515g&link_type=abstract

SF2A-2005: Semaine de l'Astrophysique Francaise, meeting held in Strasbourg, France, June 27 - July 1, 2005, Edited by F. Casoli

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We perform detailed radiative transfer modeling of the emission expected from magnetic flares in Active Galactic Nuclei (AGN). We assume a compact flare source above the accretion disk surrounding a supermassive black hole. The source is supposed to be anchored in the disk by magnetic structures and orbits around the center on Keplerian time scales. For the spectral modeling we take into account the primary radiation coming directly from the flare source and a Compton reflection/reprocessed component coming from the disk surface. The disk is supposed to be in hydrostatic equilibrium. Its density, temperature and ionization profiles are computed self-consistently. We take into account the variations of the incident radiation across the hot-spot underneath the flare source. We analyze the spectra emitted at the flare location for different emission directions. We then conduct relativistic ray tracing to obtain the spectra seen by a distant observer. Our results contain time-dependent spectra and light curves for orbiting flares at various distances from the black hole. The computations are carried out for black holes of different masses and accretion rates. We also compute rms-variability spectra for large flare distributions across the disk. Our results are compared to observed data of MCG -6-30-15.

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