Relative alignment between dense molecular cores and ambient magnetic field: the synergy of numerical models and observations
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- Che-Yu Chen
- Department of Astronomy, University of Virginia, Charlottesville, VA 22904, USA
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- Erica A Behrens
- Department of Astronomy, Ohio State University, Columbus, OH 43210, USA
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- Jasmin E Washington
- Department of Astronomy, University of Virginia, Charlottesville, VA 22904, USA
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- Laura M Fissel
- National Radio Astronomy Observatory, Charlottesville, VA 22904, USA
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- Rachel K Friesen
- National Radio Astronomy Observatory, Charlottesville, VA 22904, USA
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- Zhi-Yun Li
- Department of Astronomy, University of Virginia, Charlottesville, VA 22904, USA
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- Jaime E Pineda
- Max-Planck-Institut für extraterrestrische Physik, Giessenbachstrasse 1, D-85748 Garching, Germany
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- Adam Ginsburg
- Department of Astronomy, University of Florida, Gainesville, FL 32611, USA
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- Helen Kirk
- Herzberg Astronomy and Astrophysics, National Research Council of Canada, Victoria, BC V9E 2E7, Canada
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- Samantha Scibelli
- Department of Astronomy, University of Arizona, Tucson, AZ 85721, USA
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- Felipe Alves
- Max-Planck-Institut für extraterrestrische Physik, Giessenbachstrasse 1, D-85748 Garching, Germany
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- Elena Redaelli
- Max-Planck-Institut für extraterrestrische Physik, Giessenbachstrasse 1, D-85748 Garching, Germany
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- Paola Caselli
- Max-Planck-Institut für extraterrestrische Physik, Giessenbachstrasse 1, D-85748 Garching, Germany
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- Anna Punanova
- Ural Federal University, Mira St 19, Yekaterinburg 620002, Russia
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- James Di Francesco
- Herzberg Astronomy and Astrophysics, National Research Council of Canada, Victoria, BC V9E 2E7, Canada
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- Erik Rosolowsky
- Department of Physics, University of Alberta, Edmonton, AB T6G 2E1, Canada
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- Stella S R Offner
- Department of Astronomy, University of Texas at Austin, Austin, TX 78712, USA
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- Peter G Martin
- Canadian Institute for Theoretical Astrophysics, University of Toronto, Toronto, ON M5S 3H8, Canada
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- Ana Chacón-Tanarro
- Observatorio Astronómico Nacional (OAN-IGN), Alfonso XII 3, E-28014 Madrid, Spain
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- Hope H-H Chen
- Department of Astronomy, University of Texas at Austin, Austin, TX 78712, USA
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- Michael C-Y Chen
- Department of Physics, University of Alberta, Edmonton, AB T6G 2E1, Canada
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- Jared Keown
- Department of Physics, University of Alberta, Edmonton, AB T6G 2E1, Canada
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- Youngmin Seo
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA
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- Yancy Shirley
- Department of Astronomy, University of Arizona, Tucson, AZ 85721, USA
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- Hector G Arce
- Department of Astronomy, Yale University, New Haven, CT 06520, USA
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- Alyssa A Goodman
- Harvard–Smithsonian Center for Astrophysics, Cambridge, MA 02138, USA
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- Christopher D Matzner
- Department of Astronomy & Astrophysics, University of Toronto, Toronto, ON M5S 3H4, Canada
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- Philip C Myers
- Harvard–Smithsonian Center for Astrophysics, Cambridge, MA 02138, USA
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- Ayushi Singh
- Department of Astronomy & Astrophysics, University of Toronto, Toronto, ON M5S 3H4, Canada
抄録
<jats:title>ABSTRACT</jats:title> <jats:p>The role played by magnetic field during star formation is an important topic in astrophysics. We investigate the correlation between the orientation of star-forming cores (as defined by the core major axes) and ambient magnetic field directions in (i) a 3D magnetohydrodynamic simulation, (ii) synthetic observations generated from the simulation at different viewing angles, and (iii) observations of nearby molecular clouds. We find that the results on relative alignment between cores and background magnetic field in synthetic observations slightly disagree with those measured in fully 3D simulation data, which is partly because cores identified in projected 2D maps tend to coexist within filamentary structures, while 3D cores are generally more rounded. In addition, we examine the progression of magnetic field from pc to core scale in the simulation, which is consistent with the anisotropic core formation model that gas preferably flows along the magnetic field towards dense cores. When comparing the observed cores identified from the Green Bank Ammonia Survey and Planck polarization-inferred magnetic field orientations, we find that the relative core–field alignment has a regional dependence among different clouds. More specifically, we find that dense cores in the Taurus molecular cloud tend to align perpendicular to the background magnetic field, while those in Perseus and Ophiuchus tend to have random (Perseus) or slightly parallel (Ophiuchus) orientations with respect to the field. We argue that this feature of relative core–field orientation could be used to probe the relative significance of the magnetic field within the cloud.</jats:p>
収録刊行物
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- Monthly Notices of the Royal Astronomical Society
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Monthly Notices of the Royal Astronomical Society 494 (2), 1971-1987, 2020-03-28
Oxford University Press (OUP)