A magnetohydrodynamic nonradiative accretion flow in three dimensions
We present a global magnetohydrodynamic (MHD) three-dimensional simulation of a nonradiative accretion flow originating in a pressure-supported torus. The evolution is controlled by the magnetorotational instability, which produces turbulence. The flow forms a nearly Keplerian disk. The total pressu...
| Main Authors: | , , |
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| Format: | Journal article |
| Language: | English |
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Institute of Physics Publishing
2001
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| _version_ | 1797071393866645504 |
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| author | Hawley, J Balbus, SA Stone, J |
| author_facet | Hawley, J Balbus, SA Stone, J |
| author_sort | Hawley, J |
| collection | OXFORD |
| description | We present a global magnetohydrodynamic (MHD) three-dimensional simulation of a nonradiative accretion flow originating in a pressure-supported torus. The evolution is controlled by the magnetorotational instability, which produces turbulence. The flow forms a nearly Keplerian disk. The total pressure scale height in this disk is comparable to the vertical size of the initial torus. Gas pressure dominates near the equator; magnetic pressure is more important in the surrounding atmosphere. A magnetically dominated bound outflow is driven from the disk. The accretion rate through the disk exceeds the final rate into the hole, and a hot torus forms inside 10rg. Hot gas, pushed up against the centrifugal barrier and confined by magnetic pressure, is ejected in a narrow, unbound, conical outflow. The dynamics are controlled by magnetic turbulence, not thermal convection, and a hydrodynamic α-model is inadequate to describe the flow. The limitations of two-dimensional MHD simulations are also discussed. |
| first_indexed | 2024-03-06T22:52:35Z |
| format | Journal article |
| id | oxford-uuid:5f4b4375-9ac9-45c2-92e3-fa068b6f98e6 |
| institution | University of Oxford |
| language | English |
| last_indexed | 2024-03-06T22:52:35Z |
| publishDate | 2001 |
| publisher | Institute of Physics Publishing |
| record_format | dspace |
| spelling | oxford-uuid:5f4b4375-9ac9-45c2-92e3-fa068b6f98e62022-03-26T17:46:00ZA magnetohydrodynamic nonradiative accretion flow in three dimensionsJournal articlehttp://purl.org/coar/resource_type/c_dcae04bcuuid:5f4b4375-9ac9-45c2-92e3-fa068b6f98e6EnglishSymplectic Elements at OxfordInstitute of Physics Publishing2001Hawley, JBalbus, SAStone, JWe present a global magnetohydrodynamic (MHD) three-dimensional simulation of a nonradiative accretion flow originating in a pressure-supported torus. The evolution is controlled by the magnetorotational instability, which produces turbulence. The flow forms a nearly Keplerian disk. The total pressure scale height in this disk is comparable to the vertical size of the initial torus. Gas pressure dominates near the equator; magnetic pressure is more important in the surrounding atmosphere. A magnetically dominated bound outflow is driven from the disk. The accretion rate through the disk exceeds the final rate into the hole, and a hot torus forms inside 10rg. Hot gas, pushed up against the centrifugal barrier and confined by magnetic pressure, is ejected in a narrow, unbound, conical outflow. The dynamics are controlled by magnetic turbulence, not thermal convection, and a hydrodynamic α-model is inadequate to describe the flow. The limitations of two-dimensional MHD simulations are also discussed. |
| spellingShingle | Hawley, J Balbus, SA Stone, J A magnetohydrodynamic nonradiative accretion flow in three dimensions |
| title | A magnetohydrodynamic nonradiative accretion flow in three dimensions |
| title_full | A magnetohydrodynamic nonradiative accretion flow in three dimensions |
| title_fullStr | A magnetohydrodynamic nonradiative accretion flow in three dimensions |
| title_full_unstemmed | A magnetohydrodynamic nonradiative accretion flow in three dimensions |
| title_short | A magnetohydrodynamic nonradiative accretion flow in three dimensions |
| title_sort | magnetohydrodynamic nonradiative accretion flow in three dimensions |
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