Astronomy and Astrophysics – Astronomy
Scientific paper
Dec 2003
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003aas...20310405j&link_type=abstract
American Astronomical Society Meeting 203, #104.05; Bulletin of the American Astronomical Society, Vol. 35, p.1373
Astronomy and Astrophysics
Astronomy
Scientific paper
We calculate the strength, profiles, and emissivities of the X-ray emission lines expected for an accretion disk orbiting a supermassive Kerr black hole. We find that the O VIII, N VII, and C VI lines detected with XMM-Newton in the active galaxy MCG-6-30-15 by Branduardi-Raymont et al. (2001) are physically tenable, but are brighter than calculated in our model. Also, the model lines include O VII emission with no strong N VII. We find that atmospheric effects can steepen the emissivities for the Fe XXVI and Fe XXV lines. Also, we predict an anti-correlation between the Fe K fluorescence and the soft X-ray line intensities. X-ray opacity, Compton scattering, and dynamical effects become crucial for calculating the line spectrum. We are in the process of adding line transfer in the model via a Monte Carlo, and we find that the line ratios will be substantially modified after repeated photoionizations and recombinations inside the atmosphere. The result is the enhancement of the O VIII (654 eV) and C VI (367 eV) line fluxes by 44% and 105%.
Jimenez-Garate Mario A.
Liedahl Duane Allen
Mathiesen Benjamin F.
Mauche Christopher W.
Raymond John C.
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