The CARMA-NRO Orion Survey: Filament Formation via Collision-Induced Magnetic Reconnection -- The Stick in Orion A
A unique filament is identified in the {\it 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 show...
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| creator | Kong, Shuo Ossenkopf-Okada, Volker Arce, Héctor G Bally, John Sánchez-Monge, Álvaro McGehee, Peregrine Suri, Sümeyye Klessen, Ralf S Carpenter, John M Lis, Dariusz C Nakamura, Fumitaka Schilke, Peter Smith, Rowan J Mairs, Steve Goodman, Alyssa Maureira, María José |
| description | A unique filament is identified in the {\it 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 C\(^{18}\)O(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 (MHD) code Athena++ to simulate the collision between two diffuse molecular clumps, each carrying an anti-parallel 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 free-fall 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. |
| doi_str_mv | 10.48550/arxiv.2011.00183 |
| format | Article |
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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 C\(^{18}\)O(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 (MHD) code Athena++ to simulate the collision between two diffuse molecular clumps, each carrying an anti-parallel 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 free-fall collapse. The dense filament shows ring/fork-like structures in radiative transfer maps. Cores in the filament are confined by surface magnetic pressure. 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CMR can be an important dense-gas-producing mechanism in the Galaxy and beyond.</description><subject>Clumps</subject><subject>Fluid dynamics</subject><subject>Galaxies</subject><subject>Magnetohydrodynamics</subject><subject>Molecular clouds</subject><subject>Physics - Astrophysics of Galaxies</subject><subject>Physics - Solar and Stellar Astrophysics</subject><subject>Radiative transfer</subject><issn>2331-8422</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2020</creationdate><recordtype>article</recordtype><sourceid>ABUWG</sourceid><sourceid>AFKRA</sourceid><sourceid>AZQEC</sourceid><sourceid>BENPR</sourceid><sourceid>CCPQU</sourceid><sourceid>DWQXO</sourceid><sourceid>GOX</sourceid><recordid>eNotkE1rwkAQhpdCoWL9AT11oee1-5mNvYVQW0EraO5hslnbtXFjN4nov2_8OA3D-_Ay8yD0xOhYxkrRVwhHdxhzytiYUhaLOzTgQjASS84f0KhptpRSHmmulBigkP1YnCarRUK-Vku8DK72eN2Fgz294amrYGd9i6d12EF7jg4OcFpXlWv6jcx82Rlb4gV8e9s6g1fW1N5bc2EJwef2dR_8Yudv5ckjut9A1djRbQ5RNn3P0k8yX37M0mROQHFGpNZCw0ZTDsZAITiPpIZJaZQuNd-UJi5ATUzRv2gjbSNBjTLSgADTAyoWQ_R8rb0IyffB7SCc8rOY_CKmJ16uxD7Uf51t2nxbd8H3N-VcKs2k4oKJfxJiZOs</recordid><startdate>20201031</startdate><enddate>20201031</enddate><creator>Kong, Shuo</creator><creator>Ossenkopf-Okada, Volker</creator><creator>Arce, Héctor G</creator><creator>Bally, John</creator><creator>Sánchez-Monge, Álvaro</creator><creator>McGehee, Peregrine</creator><creator>Suri, Sümeyye</creator><creator>Klessen, Ralf S</creator><creator>Carpenter, John M</creator><creator>Lis, Dariusz C</creator><creator>Nakamura, Fumitaka</creator><creator>Schilke, Peter</creator><creator>Smith, Rowan J</creator><creator>Mairs, Steve</creator><creator>Goodman, Alyssa</creator><creator>Maureira, María José</creator><general>Cornell University Library, arXiv.org</general><scope>8FE</scope><scope>8FG</scope><scope>ABJCF</scope><scope>ABUWG</scope><scope>AFKRA</scope><scope>AZQEC</scope><scope>BENPR</scope><scope>BGLVJ</scope><scope>CCPQU</scope><scope>DWQXO</scope><scope>HCIFZ</scope><scope>L6V</scope><scope>M7S</scope><scope>PIMPY</scope><scope>PQEST</scope><scope>PQQKQ</scope><scope>PQUKI</scope><scope>PRINS</scope><scope>PTHSS</scope><scope>GOX</scope></search><sort><creationdate>20201031</creationdate><title>The CARMA-NRO Orion Survey: Filament Formation via Collision-Induced Magnetic Reconnection -- The Stick in Orion A</title><author>Kong, Shuo ; 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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 C\(^{18}\)O(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 (MHD) code Athena++ to simulate the collision between two diffuse molecular clumps, each carrying an anti-parallel 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 free-fall collapse. The dense filament shows ring/fork-like structures in radiative transfer maps. Cores in the filament are confined by surface magnetic pressure. 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| subjects | Clumps Fluid dynamics Galaxies Magnetohydrodynamics Molecular clouds Physics - Astrophysics of Galaxies Physics - Solar and Stellar Astrophysics Radiative transfer |
| title | The CARMA-NRO Orion Survey: Filament Formation via Collision-Induced Magnetic Reconnection -- The Stick in Orion A |
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