Magnetic Fields in Massive Star-forming Regions (MagMaR). V. The Magnetic Field at the Onset of High-mass Star Formation
A complete understanding of the initial conditions of high-mass star formation and what processes determine multiplicity requires the study of the magnetic field in young massive cores. Using Atacama Large Millimeter/submillimeter Array (ALMA) 250 GHz polarization observations (0 $\mathop{.}\limits^...
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| author | Patricio Sanhueza Junhao Liu Kaho Morii Josep Miquel Girart Qizhou Zhang Ian W. Stephens James M. Jackson Paulo C. Cortés Patrick M. Koch Claudia J. Cyganowski Piyali Saha Henrik Beuther Suinan Zhang Maria T. Beltrán Yu Cheng Fernando A. Olguin Xing Lu Spandan Choudhury Kate Pattle Manuel Fernández-López Jihye Hwang Ji-hyun Kang Janik Karoly Adam Ginsburg A.-Ran Lyo Kotomi Taniguchi Wenyu Jiao Chakali Eswaraiah Qiu-yi Luo Jia-Wei Wang Benoît Commerçon Shanghuo Li Fengwei Xu Huei-Ru Vivien Chen Luis A. Zapata Eun Jung Chung Fumitaka Nakamura Sandhyarani Panigrahy Takeshi Sakai |
| author_facet | Patricio Sanhueza Junhao Liu Kaho Morii Josep Miquel Girart Qizhou Zhang Ian W. Stephens James M. Jackson Paulo C. Cortés Patrick M. Koch Claudia J. Cyganowski Piyali Saha Henrik Beuther Suinan Zhang Maria T. Beltrán Yu Cheng Fernando A. Olguin Xing Lu Spandan Choudhury Kate Pattle Manuel Fernández-López Jihye Hwang Ji-hyun Kang Janik Karoly Adam Ginsburg A.-Ran Lyo Kotomi Taniguchi Wenyu Jiao Chakali Eswaraiah Qiu-yi Luo Jia-Wei Wang Benoît Commerçon Shanghuo Li Fengwei Xu Huei-Ru Vivien Chen Luis A. Zapata Eun Jung Chung Fumitaka Nakamura Sandhyarani Panigrahy Takeshi Sakai |
| author_sort | Patricio Sanhueza |
| collection | DOAJ |
| description | A complete understanding of the initial conditions of high-mass star formation and what processes determine multiplicity requires the study of the magnetic field in young massive cores. Using Atacama Large Millimeter/submillimeter Array (ALMA) 250 GHz polarization observations (0 $\mathop{.}\limits^{^{\prime\prime} }$ 3 = 1000 au) and ALMA 220 GHz high-angular-resolution observations (0 $\mathop{.}\limits^{^{\prime\prime} }$ 05 = 160 au), we have performed a full energy analysis including the magnetic field at core scales and have assessed what influences the multiplicity inside a massive core previously believed to be in the prestellar phase. With a mass of 31 M _⊙ , the G11.92 MM2 core has a young CS molecular outflow with a dynamical timescale of a few thousand years. At high resolution, the MM2 core fragments into a binary system, with a projected separation of 505 au and a binary mass ratio of 1.14. Using the Davis–Chandrasekhar–Fermi method with an angle dispersion function analysis, we estimate in this core a magnetic field strength of 6.2 mG and a mass-to-magnetic-flux ratio of 18. The MM2 core is strongly subvirialized, with a virial parameter of 0.064, including the magnetic field. The high mass-to-magnetic-flux ratio and low virial parameter indicate that this massive core is very likely undergoing runaway collapse, which is in direct contradiction with the core accretion model. The MM2 core is embedded in a filament that has a velocity gradient consistent with infall. In line with clump-fed scenarios, the core can grow in mass at a rate of 1.9–5.6 × 10 ^−4 M _⊙ yr ^−1 . In spite of the magnetic field having only a minor contribution to the total energy budget at core scales (a few thousands of astronomical units), it likely plays a more important role at smaller scales (a few hundreds of astronomical units) by setting the binary properties. Considering energy ratios and a fragmentation criterion at the core scale, the binary system could have been formed by core fragmentation. The binary system properties (projected separation and mass ratio), however, are also consistent with radiation-magnetohydrodynamic simulations with super-Alfvenic or supersonic (or sonic) turbulence that form binaries by disk fragmentation. |
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| institution | DOAJ |
| issn | 1538-4357 |
| language | English |
| publishDate | 2025-01-01 |
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| spelling | doaj-art-6f4991e02fa64afb83a7fe402b5e88902025-08-20T03:00:45ZengIOP PublishingThe Astrophysical Journal1538-43572025-01-0198018710.3847/1538-4357/ad9d40Magnetic Fields in Massive Star-forming Regions (MagMaR). V. The Magnetic Field at the Onset of High-mass Star FormationPatricio Sanhueza0https://orcid.org/0000-0002-7125-7685Junhao Liu1https://orcid.org/0000-0002-4774-2998Kaho Morii2https://orcid.org/0000-0002-6752-6061Josep Miquel Girart3https://orcid.org/0000-0002-3829-5591Qizhou Zhang4https://orcid.org/0000-0003-2384-6589Ian W. Stephens5https://orcid.org/0000-0003-3017-4418James M. Jackson6https://orcid.org/0000-0002-3466-6164Paulo C. Cortés7https://orcid.org/0000-0002-3583-780XPatrick M. Koch8https://orcid.org/0000-0003-2777-5861Claudia J. Cyganowski9https://orcid.org/0000-0001-6725-1734Piyali Saha10https://orcid.org/0000-0002-0028-1354Henrik Beuther11https://orcid.org/0000-0002-1700-090XSuinan Zhang12https://orcid.org/0000-0002-8389-6695Maria T. Beltrán13https://orcid.org/0000-0003-3315-5626Yu Cheng14https://orcid.org/0000-0002-8691-4588Fernando A. Olguin15https://orcid.org/0000-0002-8250-6827Xing Lu16https://orcid.org/0000-0003-2619-9305Spandan Choudhury17https://orcid.org/0000-0002-7497-2713Kate Pattle18https://orcid.org/0000-0002-8557-3582Manuel Fernández-López19https://orcid.org/0000-0001-5811-0454Jihye Hwang20https://orcid.org/0000-0001-7866-2686Ji-hyun Kang21https://orcid.org/0000-0001-7379-6263Janik Karoly22https://orcid.org/0000-0001-5996-3600Adam Ginsburg23https://orcid.org/0000-0001-6431-9633A.-Ran Lyo24https://orcid.org/0000-0002-9907-8427Kotomi Taniguchi25https://orcid.org/0000-0003-4402-6475Wenyu Jiao26https://orcid.org/0000-0001-9822-7817Chakali Eswaraiah27https://orcid.org/0000-0003-4761-6139Qiu-yi Luo28https://orcid.org/0000-0003-4506-3171Jia-Wei Wang29https://orcid.org/0000-0002-6668-974XBenoît Commerçon30https://orcid.org/0000-0003-2407-1025Shanghuo Li31https://orcid.org/0000-0003-1275-5251Fengwei Xu32https://orcid.org/0000-0001-5950-1932Huei-Ru Vivien Chen33https://orcid.org/0000-0002-9774-1846Luis A. Zapata34https://orcid.org/0000-0003-2343-7937Eun Jung Chung35https://orcid.org/0000-0003-0014-1527Fumitaka Nakamura36https://orcid.org/0009-0007-6357-6874Sandhyarani Panigrahy37https://orcid.org/0000-0001-5431-2294Takeshi Sakai38https://orcid.org/0000-0003-4521-7492Department of Earth and Planetary Sciences , Institute of Science Tokyo, Meguro, Tokyo 152-8551, Japan ; patosanhueza@gmail.com; National Astronomical Observatory of Japan , National Institutes of Natural Sciences, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan; Department of Astronomical Science, SOKENDAI (The Graduate University for Advanced Studies) , 2-21-1 Osawa, Mitaka, Tokyo 181-8588, JapanNational Astronomical Observatory of Japan , National Institutes of Natural Sciences, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, JapanNational Astronomical Observatory of Japan , National Institutes of Natural Sciences, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan; Department of Astronomy, Graduate School of Science, The University of Tokyo , 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033, JapanInstitut de Ciències de l’Espai (ICE, CSIC) , Can Magrans s/n, 08193, Cerdanyola del Vallés, Catalonia, Spain; Institut d’Estudis Espacials de Catalunya (IEEC) , 08034, Barcelona, Catalonia, SpainCenter for Astrophysics ∣Harvard & Smithsonian , 60 Garden Street, Cambridge, MA 02138, USADepartment of Earth, Environment, and Physics, Worcester State University , Worcester, MA 01602, USAGreen Bank Observatory , 155 Observatory Road, Green Bank, WV 24944, USAJoint ALMA Observatory , Alonso de Córdova 3107, Vitacura, Santiago, Chile; National Radio Astronomy Observatory , 520 Edgemont Road, Charlottesville, VA 22903, USAAcademia Sinica , Institute of Astronomy and Astrophysics, No.1, Sec. 4, Roosevelt Road, Taipei 10617, TaiwanSUPA, School of Physics and Astronomy, University of St. Andrews , North Haugh, St. Andrews, KY16 9SS, UKNational Astronomical Observatory of Japan , National Institutes of Natural Sciences, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, JapanMax Planck Institute for Astronomy , Königstuhl 17, 69117 Heidelberg, GermanyShanghai Astronomical Observatory , Chinese Academy of Sciences, 80 Nandan Road, Shanghai 200030, People’s Republic of ChinaINAF-Osservatorio Astrofisico di Arcetri , Largo E. Fermi 5, I-50125 Firenze, ItalyNational Astronomical Observatory of Japan , National Institutes of Natural Sciences, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, JapanNational Astronomical Observatory of Japan , National Institutes of Natural Sciences, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan; Yukawa Institute for Theoretical Physics, Kyoto University , Kyoto 606-8502, Japan; Institute of Astronomy and Department of Physics, National Tsing Hua University , Hsinchu 300044, TaiwanShanghai Astronomical Observatory , Chinese Academy of Sciences, 80 Nandan Road, Shanghai 200030, People’s Republic of ChinaKorea Astronomy and Space Science Institute (KASI) , 776 Daedeokdae-ro, Yuseong-gu, Daejeon 34055, Republic of KoreaDepartment of Physics and Astronomy, University College London , Gower Street, London, WC1E 6BT, UKInstituto Argentino de Radioastronomía (CCT- La Plata, CONICET, CICPBA, UNLP) , C.C. No. 5, 1894, Villa Elisa, Buenos Aires, ArgentinaKorea Astronomy and Space Science Institute (KASI) , 776 Daedeokdae-ro, Yuseong-gu, Daejeon 34055, Republic of KoreaKorea Astronomy and Space Science Institute (KASI) , 776 Daedeokdae-ro, Yuseong-gu, Daejeon 34055, Republic of KoreaDepartment of Physics and Astronomy, University College London , Gower Street, London, WC1E 6BT, UKDepartment of Astronomy, University of Florida , P.O. Box 112055, Gainesville, FL 32611, USAKorea Astronomy and Space Science Institute (KASI) , 776 Daedeokdae-ro, Yuseong-gu, Daejeon 34055, Republic of KoreaNational Astronomical Observatory of Japan , National Institutes of Natural Sciences, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, JapanShanghai Astronomical Observatory , Chinese Academy of Sciences, 80 Nandan Road, Shanghai 200030, People’s Republic of ChinaDepartment of Physics , Indian Institute of Science Education and Research (IISER) Tirupati, Yerpedu, Tirupati - 517619, Andhra Pradesh, IndiaShanghai Astronomical Observatory , Chinese Academy of Sciences, 80 Nandan Road, Shanghai 200030, People’s Republic of China; School of Astronomy and Space Sciences, University of Chinese Academy of Sciences , No. 19A Yuquan Road, Beijing 100049, People’s Republic of China; Key Laboratory of Radio Astronomy and Technology , Chinese Academy of Sciences, A20 Datun Road, Chaoyang District, Beijing 100101, People’s Republic of ChinaAcademia Sinica , Institute of Astronomy and Astrophysics, No.1, Sec. 4, Roosevelt Road, Taipei 10617, Taiwan; East Asian Observatory, 660 N. A’ohōkū Place, University Park , Hilo, HI 96720, USAUniv. Lyon , Ens de Lyon, Univ. Lyon 1, CNRS, Centre de Recherche Astrophysique de Lyon UMR5574, 69007, Lyon, FranceSchool of Astronomy and Space Science, Nanjing University , 163 Xianlin Avenue, Nanjing 210023, People’s Republic of China; Key Laboratory of Modern Astronomy and Astrophysics, Nanjing University , Ministry of Education, Nanjing 210023, People’s Republic of ChinaKavli Institute for Astronomy and Astrophysics, Peking University , Beijing 100871, People’s Republic of China; I. Physikalisches Institut , Universitt zu Köln, Zülpicher Str. 77, D-50937 Kln, Germany; Department of Astronomy, School of Physics, Peking University , Beijing 100871, People’s Republic of ChinaInstitute of Astronomy and Department of Physics, National Tsing Hua University , Hsinchu 300044, TaiwanInstituto de Radioastronomía y Astrofísica , Universidad Nacional Autónoma de México, P.O. Box 3-72, 58090, Morelia, Michoacán, MéxicoKorea Astronomy and Space Science Institute (KASI) , 776 Daedeokdae-ro, Yuseong-gu, Daejeon 34055, Republic of KoreaNational Astronomical Observatory of Japan , National Institutes of Natural Sciences, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan; Department of Astronomy, Graduate School of Science, The University of Tokyo , 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033, JapanDepartment of Physics , Indian Institute of Science Education and Research (IISER) Tirupati, Yerpedu, Tirupati - 517619, Andhra Pradesh, IndiaGraduate School of Informatics and Engineering, The University of Electro-Communications , Chofu, Tokyo 182-8585, JapanA complete understanding of the initial conditions of high-mass star formation and what processes determine multiplicity requires the study of the magnetic field in young massive cores. Using Atacama Large Millimeter/submillimeter Array (ALMA) 250 GHz polarization observations (0 $\mathop{.}\limits^{^{\prime\prime} }$ 3 = 1000 au) and ALMA 220 GHz high-angular-resolution observations (0 $\mathop{.}\limits^{^{\prime\prime} }$ 05 = 160 au), we have performed a full energy analysis including the magnetic field at core scales and have assessed what influences the multiplicity inside a massive core previously believed to be in the prestellar phase. With a mass of 31 M _⊙ , the G11.92 MM2 core has a young CS molecular outflow with a dynamical timescale of a few thousand years. At high resolution, the MM2 core fragments into a binary system, with a projected separation of 505 au and a binary mass ratio of 1.14. Using the Davis–Chandrasekhar–Fermi method with an angle dispersion function analysis, we estimate in this core a magnetic field strength of 6.2 mG and a mass-to-magnetic-flux ratio of 18. The MM2 core is strongly subvirialized, with a virial parameter of 0.064, including the magnetic field. The high mass-to-magnetic-flux ratio and low virial parameter indicate that this massive core is very likely undergoing runaway collapse, which is in direct contradiction with the core accretion model. The MM2 core is embedded in a filament that has a velocity gradient consistent with infall. In line with clump-fed scenarios, the core can grow in mass at a rate of 1.9–5.6 × 10 ^−4 M _⊙ yr ^−1 . In spite of the magnetic field having only a minor contribution to the total energy budget at core scales (a few thousands of astronomical units), it likely plays a more important role at smaller scales (a few hundreds of astronomical units) by setting the binary properties. Considering energy ratios and a fragmentation criterion at the core scale, the binary system could have been formed by core fragmentation. The binary system properties (projected separation and mass ratio), however, are also consistent with radiation-magnetohydrodynamic simulations with super-Alfvenic or supersonic (or sonic) turbulence that form binaries by disk fragmentation.https://doi.org/10.3847/1538-4357/ad9d40Dust continuum emissionPolarimetryStar formationStar forming regionsMassive starsMagnetic fields |
| spellingShingle | Patricio Sanhueza Junhao Liu Kaho Morii Josep Miquel Girart Qizhou Zhang Ian W. Stephens James M. Jackson Paulo C. Cortés Patrick M. Koch Claudia J. Cyganowski Piyali Saha Henrik Beuther Suinan Zhang Maria T. Beltrán Yu Cheng Fernando A. Olguin Xing Lu Spandan Choudhury Kate Pattle Manuel Fernández-López Jihye Hwang Ji-hyun Kang Janik Karoly Adam Ginsburg A.-Ran Lyo Kotomi Taniguchi Wenyu Jiao Chakali Eswaraiah Qiu-yi Luo Jia-Wei Wang Benoît Commerçon Shanghuo Li Fengwei Xu Huei-Ru Vivien Chen Luis A. Zapata Eun Jung Chung Fumitaka Nakamura Sandhyarani Panigrahy Takeshi Sakai Magnetic Fields in Massive Star-forming Regions (MagMaR). V. The Magnetic Field at the Onset of High-mass Star Formation The Astrophysical Journal Dust continuum emission Polarimetry Star formation Star forming regions Massive stars Magnetic fields |
| title | Magnetic Fields in Massive Star-forming Regions (MagMaR). V. The Magnetic Field at the Onset of High-mass Star Formation |
| title_full | Magnetic Fields in Massive Star-forming Regions (MagMaR). V. The Magnetic Field at the Onset of High-mass Star Formation |
| title_fullStr | Magnetic Fields in Massive Star-forming Regions (MagMaR). V. The Magnetic Field at the Onset of High-mass Star Formation |
| title_full_unstemmed | Magnetic Fields in Massive Star-forming Regions (MagMaR). V. The Magnetic Field at the Onset of High-mass Star Formation |
| title_short | Magnetic Fields in Massive Star-forming Regions (MagMaR). V. The Magnetic Field at the Onset of High-mass Star Formation |
| title_sort | magnetic fields in massive star forming regions magmar v the magnetic field at the onset of high mass star formation |
| topic | Dust continuum emission Polarimetry Star formation Star forming regions Massive stars Magnetic fields |
| url | https://doi.org/10.3847/1538-4357/ad9d40 |
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