TY  - GEN
N2  - We study the role of convection in black hole accretion flows. We investigate the influence of convection on the energy transport as well as the effect of convective turbulence on the disk?s viscosity. The results reveal that convection supports the radiative energy transport efficiently in massless disks, while it can turn into a negative feedback if self-gravity becomes important. Convective turbulence adds significantly to the total viscosity, but cannot account for it on its own. In the second part, we study the spectral energy distribution of super-Eddington accretion flows onto a black hole, based on 2D RHD simulation data. We model the continuum emission as well as the iron K line emission and absorption features with a ray-tracing radiative transfer code. We find that mild relativistic beaming effects become important, leading to super-Eddington luminosities for face-on seen disks. We confirm the diagnostic power of the iron K lines on the accretion process in the inner disk region, finding a strong correlation between the central black hole mass and the ratio of the K? to the K? lines. We also detect a trend of line broadening for edge-on seen disks.
A1  - Heinzeller, Dominikus
UR  - https://archiv.ub.uni-heidelberg.de/volltextserver/8575/
ID  - heidok8575
KW  - Mischungswegtheorie 
KW  -  Strahlungstransport 
KW  -  Eisen K-LinieMixing-length-theory 
KW  -  radiative transfer 
KW  -  iron K-line
AV  - public
TI  - Black hole accretion disks : sources of viscosity and signatures of super-Eddington accretion
Y1  - 2008///
ER  -