Disk modelling by radiation-magnetohydrodynamic simulations
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 th...
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EDP Sciences
2012-12-01
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Series: | EPJ Web of Conferences |
Online Access: | http://dx.doi.org/10.1051/epjconf/20123906005 |
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doaj-92861ab2b39f4447bb9aed35b57649b52021-08-02T04:04:48ZengEDP SciencesEPJ Web of Conferences2100-014X2012-12-01390600510.1051/epjconf/20123906005Disk modelling by radiation-magnetohydrodynamic simulationsTakeuchi S.Ohsuga K.Mineshige S.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. http://dx.doi.org/10.1051/epjconf/20123906005 |
collection |
DOAJ |
language |
English |
format |
Article |
sources |
DOAJ |
author |
Takeuchi S. Ohsuga K. Mineshige S. |
spellingShingle |
Takeuchi S. Ohsuga K. Mineshige S. Disk modelling by radiation-magnetohydrodynamic simulations EPJ Web of Conferences |
author_facet |
Takeuchi S. Ohsuga K. Mineshige S. |
author_sort |
Takeuchi S. |
title |
Disk modelling by radiation-magnetohydrodynamic simulations |
title_short |
Disk modelling by radiation-magnetohydrodynamic simulations |
title_full |
Disk modelling by radiation-magnetohydrodynamic simulations |
title_fullStr |
Disk modelling by radiation-magnetohydrodynamic simulations |
title_full_unstemmed |
Disk modelling by radiation-magnetohydrodynamic simulations |
title_sort |
disk modelling by radiation-magnetohydrodynamic simulations |
publisher |
EDP Sciences |
series |
EPJ Web of Conferences |
issn |
2100-014X |
publishDate |
2012-12-01 |
description |
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. |
url |
http://dx.doi.org/10.1051/epjconf/20123906005 |
work_keys_str_mv |
AT takeuchis diskmodellingbyradiationmagnetohydrodynamicsimulations AT ohsugak diskmodellingbyradiationmagnetohydrodynamicsimulations AT mineshiges diskmodellingbyradiationmagnetohydrodynamicsimulations |
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