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 pressur...
| Main Authors: | , , |
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| Format: | Journal article |
| Published: |
2001
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| _version_ | 1797054261216935936 |
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| author | Hawley, J Balbus, S Stone, J |
| author_facet | Hawley, J Balbus, S 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 only 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 10 r_g. 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 alpha model is inadequate to describe the flow. The limitations of two dimensional MHD simulations are also discussed. |
| first_indexed | 2024-03-06T18:54:43Z |
| format | Journal article |
| id | oxford-uuid:116abbe7-9594-411e-b2fb-2303ce27260d |
| institution | University of Oxford |
| last_indexed | 2024-03-06T18:54:43Z |
| publishDate | 2001 |
| record_format | dspace |
| spelling | oxford-uuid:116abbe7-9594-411e-b2fb-2303ce27260d2022-03-26T10:02:13ZA Magnetohydrodynamic Nonradiative Accretion Flow in Three DimensionsJournal articlehttp://purl.org/coar/resource_type/c_dcae04bcuuid:116abbe7-9594-411e-b2fb-2303ce27260dSymplectic Elements at Oxford2001Hawley, JBalbus, SStone, 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 only 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 10 r_g. 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 alpha model is inadequate to describe the flow. The limitations of two dimensional MHD simulations are also discussed. |
| spellingShingle | Hawley, J Balbus, S 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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