On the Magnetic Field Properties of Protostellar Envelopes in Orion
We present 870 μ m polarimetric observations toward 61 protostars in the Orion molecular clouds with ∼400 au (1″) resolution using the Atacama Large Millimeter/submillimeter Array. We successfully detect dust polarization and outflow emission in 56 protostars; in 16 of them the polarization is likel...
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| Format: | Article |
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IOP Publishing
2024-01-01
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| Series: | The Astrophysical Journal Letters |
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| Online Access: | https://doi.org/10.3847/2041-8213/ad27d4 |
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| author | Bo Huang Josep M. Girart Ian W. Stephens Manuel Fernández López Hector G. Arce John M. Carpenter Paulo Cortes Erin G. Cox Rachel Friesen Valentin J. M. Le Gouellec Charles L. H. Hull Nicole Karnath Woojin Kwon Zhi-Yun Li Leslie W. Looney S. Thomas Megeath Philip C. Myers Nadia M. Murillo Jaime E. Pineda Sarah Sadavoy Álvaro Sánchez-Monge Patricio Sanhueza John J. Tobin Qizhou Zhang James M. Jackson Dominique Segura-Cox |
| author_facet | Bo Huang Josep M. Girart Ian W. Stephens Manuel Fernández López Hector G. Arce John M. Carpenter Paulo Cortes Erin G. Cox Rachel Friesen Valentin J. M. Le Gouellec Charles L. H. Hull Nicole Karnath Woojin Kwon Zhi-Yun Li Leslie W. Looney S. Thomas Megeath Philip C. Myers Nadia M. Murillo Jaime E. Pineda Sarah Sadavoy Álvaro Sánchez-Monge Patricio Sanhueza John J. Tobin Qizhou Zhang James M. Jackson Dominique Segura-Cox |
| author_sort | Bo Huang |
| collection | DOAJ |
| description | We present 870 μ m polarimetric observations toward 61 protostars in the Orion molecular clouds with ∼400 au (1″) resolution using the Atacama Large Millimeter/submillimeter Array. We successfully detect dust polarization and outflow emission in 56 protostars; in 16 of them the polarization is likely produced by self-scattering. Self-scattering signatures are seen in several Class 0 sources, suggesting that grain growth appears to be significant in disks at earlier protostellar phases. For the rest of the protostars, the dust polarization traces the magnetic field, whose morphology can be approximately classified into three categories: standard-hourglass, rotated-hourglass (with its axis perpendicular to outflow), and spiral-like morphology. A total of 40.0% (±3.0%) of the protostars exhibit a mean magnetic field direction approximately perpendicular to the outflow on several × 10 ^2 –10 ^3 au scales. However, in the remaining sample, this relative orientation appears to be random, probably due to the complex set of morphologies observed. Furthermore, we classify the protostars into three types based on the C ^17 O (3–2) velocity envelope’s gradient: perpendicular to outflow, nonperpendicular to outflow, and unresolved gradient (≲1.0 km s ^−1 arcsec ^−1 ). In protostars with a velocity gradient perpendicular to outflow, the magnetic field lines are preferentially perpendicular to outflow, with most of them exhibiting a rotated hourglass morphology, suggesting that the magnetic field has been overwhelmed by gravity and angular momentum. Spiral-like magnetic fields are associated with envelopes having large velocity gradients, indicating that the rotation motions are strong enough to twist the field lines. All of the protostars with a standard-hourglass field morphology show no significant velocity gradient due to the strong magnetic braking. |
| first_indexed | 2024-03-07T19:12:01Z |
| format | Article |
| id | doaj.art-27821c721aab45a69205e8b99dab64a1 |
| institution | Directory Open Access Journal |
| issn | 2041-8205 |
| language | English |
| last_indexed | 2025-03-21T05:38:12Z |
| publishDate | 2024-01-01 |
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| series | The Astrophysical Journal Letters |
| spelling | doaj.art-27821c721aab45a69205e8b99dab64a12024-07-24T11:59:55ZengIOP PublishingThe Astrophysical Journal Letters2041-82052024-01-019631L3110.3847/2041-8213/ad27d4On the Magnetic Field Properties of Protostellar Envelopes in OrionBo Huang0https://orcid.org/0000-0001-7393-8583Josep M. Girart1https://orcid.org/0000-0002-3829-5591Ian W. Stephens2https://orcid.org/0000-0003-3017-4418Manuel Fernández López3https://orcid.org/0000-0001-5811-0454Hector G. Arce4https://orcid.org/0000-0001-5653-7817John M. Carpenter5https://orcid.org/0000-0003-2251-0602Paulo Cortes6https://orcid.org/0000-0002-3583-780XErin G. Cox7https://orcid.org/0000-0002-5216-8062Rachel Friesen8https://orcid.org/0000-0001-7594-8128Valentin J. M. Le Gouellec9https://orcid.org/0000-0002-5714-799XCharles L. H. Hull10https://orcid.org/0000-0002-8975-7573Nicole Karnath11https://orcid.org/0000-0003-3682-854XWoojin Kwon12https://orcid.org/0000-0003-4022-4132Zhi-Yun Li13https://orcid.org/0000-0002-7402-6487Leslie W. Looney14https://orcid.org/0000-0002-4540-6587S. Thomas Megeath15https://orcid.org/0000-0001-7629-3573Philip C. Myers16https://orcid.org/0000-0002-2885-1806Nadia M. Murillo17Jaime E. Pineda18https://orcid.org/0000-0002-3972-1978Sarah Sadavoy19https://orcid.org/0000-0001-7474-6874Álvaro Sánchez-Monge20https://orcid.org/0000-0002-3078-9482Patricio Sanhueza21https://orcid.org/0000-0002-7125-7685John J. Tobin22https://orcid.org/0000-0002-6195-0152Qizhou Zhang23https://orcid.org/0000-0003-2384-6589James M. Jackson24https://orcid.org/0000-0002-3466-6164Dominique Segura-Cox25https://orcid.org/0000-0003-3172-6763Institut de Ciències de l’Espai (ICE-CSIC) , Campus UAB, Can Magrans S/N, E-08193 Cerdanyola del Vallès, Catalonia, Spain ; huang@ice.csic.es, girart@ieec.catInstitut de Ciències de l’Espai (ICE-CSIC) , Campus UAB, Can Magrans S/N, E-08193 Cerdanyola del Vallès, Catalonia, Spain ; huang@ice.csic.es, girart@ieec.cat; Institut d’Estudis Espacials de Catalunya (IEEC) , c/Gran Capita, 2-4, E-08034 Barcelona, Catalonia, SpainDepartment of Earth, Environment, and Physics, Worcester State University , Worcester, MA 01602, USAInstituto Argentino de Radioastronomía (CCT-La Plata , CONICET; CICPBA), C.C. No. 5, 1894, Villa Elisa, Buenos Aires, ArgentinaDepartment of Astronomy, Yale University , New Haven, CT 06511, USAJoint ALMA Observatory , Av. Alonso de Córdova 3107, Vitacura, Santiago, ChileNational Radio Astronomy Observatory , 520 Edgemont Rd., Charlottesville, VA 22093, USA; Joint ALMA Observatory , Alonso de Córdova 3107, Vitacura, Santiago, ChileCenter for Interdisciplinary Exploration and Research in Astrophysics (CIERA) , 1800 Sherman Avenue, Evanston, IL 60201, USADepartment of Astronomy & Astrophysics, University of Toronto , 50 St. George St., Toronto, ON M5S 3H4, CanadaNASA Ames Research Center , Space Science and Astrobiology Division M.S. 245-6 Moffett Field, CA 94035, USAJoint ALMA Observatory , Av. Alonso de Córdova 3107, Vitacura, Santiago, Chile; National Astronomical Observatory of Japan , Alonso de Córdova 3788, Office 61B, Vitacura, Santiago, ChileSOFIA Science Center, Universities Space Research Association , NASA Ames Research Center, Moffett Field, CA 94035, USA; Space Science Institute , 4765 Walnut St., Suite B Boulder, CO 80301, USA; Center for Astrophysics ∣ Harvard & Smithsonian, 60 Garden Street, Cambridge, MA 02138, USADepartment of Earth Science Education, Seoul National University , 1 Gwanak-ro, Gwanak-gu, Seoul 08826, Republic of Korea; SNU Astronomy Research Center, Seoul National University , 1 Gwanak-ro, Gwanak-gu, Seoul 08826, Republic of KoreaAstronomy Department, University of Virginia , Charlottesville, VA 22904, USADepartment of Astronomy, University of Illinois , 1002 West Green Street, Urbana, IL 61801, USADepartment of Physics and Astronomy, University of Toledo , Toledo, OH 43606, USACenter for Astrophysics ∣ Harvard & Smithsonian, 60 Garden Street, Cambridge, MA 02138, USAInstituto de Astronomía, Universidad Nacional Autónoma de México , AP106, Ensenada CP 22830, B.C., México; Star and Planet Formation Laboratory, RIKEN Cluster for Pioneering Research , Wako, Saitama 351-0198, JapanCenter for Astrochemical Studies , Max Planck Institute for Extraterrestrial Physics, D-85748 Garching, GermanyDepartment of Physics, Engineering and Astronomy, Queen's University , 64 Bader Lane, Kingston, ON K7L 3N6, CanadaInstitut de Ciències de l’Espai (ICE-CSIC) , Campus UAB, Can Magrans S/N, E-08193 Cerdanyola del Vallès, Catalonia, Spain ; huang@ice.csic.es, girart@ieec.cat; Institut d’Estudis Espacials de Catalunya (IEEC) , c/Gran Capita, 2-4, E-08034 Barcelona, Catalonia, SpainNational Astronomical Observatory of Japan , 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan; Astronomical Science Program, The Graduate University for Advanced Studies , SOKENDAI, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, JapanNational Radio Astronomy Observatory , 520 Edgemont Rd., Charlottesville, VA 22093, USACenter for Astrophysics ∣ Harvard & Smithsonian, 60 Garden Street, Cambridge, MA 02138, USANational Radio Astronomy Observatory , 520 Edgemont Rd., Charlottesville, VA 22093, USACenter for Astrochemical Studies , Max Planck Institute for Extraterrestrial Physics, D-85748 Garching, Germany; Department of Astronomy, University of Texas , 2515 Speedway, Stop C1400, Austin, TX 78712, USAWe present 870 μ m polarimetric observations toward 61 protostars in the Orion molecular clouds with ∼400 au (1″) resolution using the Atacama Large Millimeter/submillimeter Array. We successfully detect dust polarization and outflow emission in 56 protostars; in 16 of them the polarization is likely produced by self-scattering. Self-scattering signatures are seen in several Class 0 sources, suggesting that grain growth appears to be significant in disks at earlier protostellar phases. For the rest of the protostars, the dust polarization traces the magnetic field, whose morphology can be approximately classified into three categories: standard-hourglass, rotated-hourglass (with its axis perpendicular to outflow), and spiral-like morphology. A total of 40.0% (±3.0%) of the protostars exhibit a mean magnetic field direction approximately perpendicular to the outflow on several × 10 ^2 –10 ^3 au scales. However, in the remaining sample, this relative orientation appears to be random, probably due to the complex set of morphologies observed. Furthermore, we classify the protostars into three types based on the C ^17 O (3–2) velocity envelope’s gradient: perpendicular to outflow, nonperpendicular to outflow, and unresolved gradient (≲1.0 km s ^−1 arcsec ^−1 ). In protostars with a velocity gradient perpendicular to outflow, the magnetic field lines are preferentially perpendicular to outflow, with most of them exhibiting a rotated hourglass morphology, suggesting that the magnetic field has been overwhelmed by gravity and angular momentum. Spiral-like magnetic fields are associated with envelopes having large velocity gradients, indicating that the rotation motions are strong enough to twist the field lines. All of the protostars with a standard-hourglass field morphology show no significant velocity gradient due to the strong magnetic braking.https://doi.org/10.3847/2041-8213/ad27d4Star formationMagnetic fieldsProtostars |
| spellingShingle | Bo Huang Josep M. Girart Ian W. Stephens Manuel Fernández López Hector G. Arce John M. Carpenter Paulo Cortes Erin G. Cox Rachel Friesen Valentin J. M. Le Gouellec Charles L. H. Hull Nicole Karnath Woojin Kwon Zhi-Yun Li Leslie W. Looney S. Thomas Megeath Philip C. Myers Nadia M. Murillo Jaime E. Pineda Sarah Sadavoy Álvaro Sánchez-Monge Patricio Sanhueza John J. Tobin Qizhou Zhang James M. Jackson Dominique Segura-Cox On the Magnetic Field Properties of Protostellar Envelopes in Orion The Astrophysical Journal Letters Star formation Magnetic fields Protostars |
| title | On the Magnetic Field Properties of Protostellar Envelopes in Orion |
| title_full | On the Magnetic Field Properties of Protostellar Envelopes in Orion |
| title_fullStr | On the Magnetic Field Properties of Protostellar Envelopes in Orion |
| title_full_unstemmed | On the Magnetic Field Properties of Protostellar Envelopes in Orion |
| title_short | On the Magnetic Field Properties of Protostellar Envelopes in Orion |
| title_sort | on the magnetic field properties of protostellar envelopes in orion |
| topic | Star formation Magnetic fields Protostars |
| url | https://doi.org/10.3847/2041-8213/ad27d4 |
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