EPJ Web of Conferences
Volume 39, 2012Tidal Disruption Events and AGN Outbursts
|Number of page(s)||4|
|Section||AGN Outbursts and Accretion Physics|
|Published online||18 December 2012|
Disk modelling by radiation-magnetohydrodynamic simulations
1 Department of Astronomy, Graduate School of Sciences, Kyoto University, Kyoto 606-8502, Japan
2 Theory Division, National Astronomical Observatory, Mitaka, Tokyo 181-8588, Japan
Historically, various accretion models have been discussed under radially one-zone approximations. In such one-zone models, however, dynamical aspects of the accretion flow, such as internal circulation and outflows, have been totally neglected. Further, the disk viscosity is usually described by the phenomenological α-viscosity model. We, here, elucidate the theory of accretion flows and outflows based on our global, two-dimensional radiation-magnetohydrodynamic simulations, not relying on the α model. We have succeeded in producing three distinct states of accretion flow by controling only one parameter, a density normalization. Of particular importance is the presence of outflows in all three states. Several noteworthy features of the supercritical (or super-Eddington) accretion flows are found; that is, relativistic, collimated outflows (jets), and low-velocity, uncollimated outflows with clumpy structure. Observational implications are briefly discussed.
© Owned by the authors, published by EDP Sciences, 2012
This is an Open Access article distributed under the terms of the Creative Commons Attribution License 2.0, which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.
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