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M.A. Jimenez-Garate (MIT), C.W. Mauche, D.A. Liedahl (LLNL), J.C. Raymond (CfA), B.F. Mathiesen (LLNL)
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%.
The author(s) of this abstract have provided an email address for comments about the abstract: mario@alum.mit.edu
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Bulletin of the American Astronomical Society, 35#5
© 2003. The American Astronomical Soceity.