Magnetized nonlinear thin-shell instability: Numerical studies in two dimensions
We revisit the analysis of the nonlinear thin shell instability (NTSI) numerically, including magnetic fields. The magnetic tension force is expected to work against the main driver of the NTSI - namely, transverse momentum transport. However, depending on the field strength and orientation, the ins...
| Main Authors: | , , , , |
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| Format: | Journal article |
| Language: | English |
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Institute of Physics Publishing
2007
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| _version_ | 1797074779499397120 |
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| author | Heitsch, F Slyz, A Devriendt, J Hartmann, L Burkert, A |
| author_facet | Heitsch, F Slyz, A Devriendt, J Hartmann, L Burkert, A |
| author_sort | Heitsch, F |
| collection | OXFORD |
| description | We revisit the analysis of the nonlinear thin shell instability (NTSI) numerically, including magnetic fields. The magnetic tension force is expected to work against the main driver of the NTSI - namely, transverse momentum transport. However, depending on the field strength and orientation, the instability may grow. For fields aligned with the inflow, we find that the NTSI is suppressed only when the Alfvén speed surpasses the (supersonic) velocities generated along the collision interface. Even for fields perpendicular to the inflow, which are the most effective at preventing the NTSI from developing, internal structures form within the expanding slab interface, probably leading to fragmentation in the presence of self-gravity or thermal instabilities. High Reynolds numbers result in local turbulence within the perturbed slab, which in turn triggers reconnection and dissipation of the excess magnetic flux. We find that when the magnetic field is initially aligned with the flow, there exists a (weak) correlation between field strength and gas density. However, for transverse fields, this correlation essentially vanishes. In light of these results, our general conclusion is that instabilities are unlikely to be erased unless the magnetic energy in clouds is much larger than the turbulent energy. Finally, while our study is motivated by the scenario of molecular cloud formation in colliding flows, our results span a larger range of applicability, from supernova shells to colliding stellar winds. © 2007. The American Astronomical Society. All rights reserved. |
| first_indexed | 2024-03-06T23:41:08Z |
| format | Journal article |
| id | oxford-uuid:6f57fb48-f2fc-4082-84d6-d2def8524e16 |
| institution | University of Oxford |
| language | English |
| last_indexed | 2024-03-06T23:41:08Z |
| publishDate | 2007 |
| publisher | Institute of Physics Publishing |
| record_format | dspace |
| spelling | oxford-uuid:6f57fb48-f2fc-4082-84d6-d2def8524e162022-03-26T19:30:09ZMagnetized nonlinear thin-shell instability: Numerical studies in two dimensionsJournal articlehttp://purl.org/coar/resource_type/c_dcae04bcuuid:6f57fb48-f2fc-4082-84d6-d2def8524e16EnglishSymplectic Elements at OxfordInstitute of Physics Publishing2007Heitsch, FSlyz, ADevriendt, JHartmann, LBurkert, AWe revisit the analysis of the nonlinear thin shell instability (NTSI) numerically, including magnetic fields. The magnetic tension force is expected to work against the main driver of the NTSI - namely, transverse momentum transport. However, depending on the field strength and orientation, the instability may grow. For fields aligned with the inflow, we find that the NTSI is suppressed only when the Alfvén speed surpasses the (supersonic) velocities generated along the collision interface. Even for fields perpendicular to the inflow, which are the most effective at preventing the NTSI from developing, internal structures form within the expanding slab interface, probably leading to fragmentation in the presence of self-gravity or thermal instabilities. High Reynolds numbers result in local turbulence within the perturbed slab, which in turn triggers reconnection and dissipation of the excess magnetic flux. We find that when the magnetic field is initially aligned with the flow, there exists a (weak) correlation between field strength and gas density. However, for transverse fields, this correlation essentially vanishes. In light of these results, our general conclusion is that instabilities are unlikely to be erased unless the magnetic energy in clouds is much larger than the turbulent energy. Finally, while our study is motivated by the scenario of molecular cloud formation in colliding flows, our results span a larger range of applicability, from supernova shells to colliding stellar winds. © 2007. The American Astronomical Society. All rights reserved. |
| spellingShingle | Heitsch, F Slyz, A Devriendt, J Hartmann, L Burkert, A Magnetized nonlinear thin-shell instability: Numerical studies in two dimensions |
| title | Magnetized nonlinear thin-shell instability: Numerical studies in two dimensions |
| title_full | Magnetized nonlinear thin-shell instability: Numerical studies in two dimensions |
| title_fullStr | Magnetized nonlinear thin-shell instability: Numerical studies in two dimensions |
| title_full_unstemmed | Magnetized nonlinear thin-shell instability: Numerical studies in two dimensions |
| title_short | Magnetized nonlinear thin-shell instability: Numerical studies in two dimensions |
| title_sort | magnetized nonlinear thin shell instability numerical studies in two dimensions |
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