The CARMA-NRO Orion survey: filament formation via collision-induced magnetic reconnection—the Stick in Orion A
A unique filament is identified in the Herschel maps of the Orion A giant molecular cloud. The filament, which we name the Stick, is ruler-straight and at an early evolutionary stage. Transverse position-velocity diagrams show two velocity components closing in on the Stick. The filament shows conse...
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| Hauptverfasser: | , , , , , , , , , , , , , , , |
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| Dokumenttyp: | Article (Journal) |
| Sprache: | Englisch |
| Veröffentlicht: |
2021 January 11
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| In: |
The astrophysical journal
Year: 2021, Jahrgang: 906, Heft: 2 |
| ISSN: | 1538-4357 |
| DOI: | 10.3847/1538-4357/abc687 |
| Online-Zugang: | Verlag, lizenzpflichtig, Volltext: https://doi.org/10.3847/1538-4357/abc687 Verlag, lizenzpflichtig, Volltext: https://iopscience.iop.org/article/10.3847/1538-4357/abc687 
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| Verfasserangaben: | Shuo Kong, Volker Ossenkopf-Okada, Héctor G. Arce, John Bally, Álvaro Sánchez-Monge, Peregrine McGehee, Sümeyye Suri, Ralf S. Klessen, John M. Carpenter, Dariusz C. Lis, Fumitaka Nakamura, Peter Schilke, Rowan J. Smith, Steve Mairs, Alyssa Goodman, and María José Maureira |
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| 245 | 1 | 4 | |a The CARMA-NRO Orion survey |b filament formation via collision-induced magnetic reconnection—the Stick in Orion A |c Shuo Kong, Volker Ossenkopf-Okada, Héctor G. Arce, John Bally, Álvaro Sánchez-Monge, Peregrine McGehee, Sümeyye Suri, Ralf S. Klessen, John M. Carpenter, Dariusz C. Lis, Fumitaka Nakamura, Peter Schilke, Rowan J. Smith, Steve Mairs, Alyssa Goodman, and María José Maureira |
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| 520 | |a A unique filament is identified in the Herschel maps of the Orion A giant molecular cloud. The filament, which we name the Stick, is ruler-straight and at an early evolutionary stage. Transverse position-velocity diagrams show two velocity components closing in on the Stick. The filament shows consecutive rings/forks in C18O (1−0) channel maps, which is reminiscent of structures generated by magnetic reconnection. We propose that the Stick formed via collision-induced magnetic reconnection (CMR). We use the magnetohydrodynamics code Athena to simulate the collision between two diffuse molecular clumps, each carrying an antiparallel magnetic field. The clump collision produces a narrow, straight, dense filament with a factor of >200 increase in density. The production of the dense gas is seven times faster than freefall collapse. The dense filament shows ring/fork-like structures in radiative transfer maps. Cores in the filament are confined by surface magnetic pressure. CMR can be an important dense-gas-producing mechanism in the Galaxy and beyond. | ||
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| 700 | 1 | |a Nakamura, Fumitaka |e VerfasserIn |4 aut | |
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| 700 | 1 | |a Goodman, Alyssa |e VerfasserIn |4 aut | |
| 700 | 1 | |a Maureira, María José |e VerfasserIn |4 aut | |
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