Relative alignment between dense molecular cores and ambient magnetic field: the synergy of numerical models and observations

  • Che-Yu Chen
    Department of Astronomy, University of Virginia, Charlottesville, VA 22904, USA
  • Erica A Behrens
    Department of Astronomy, Ohio State University, Columbus, OH 43210, USA
  • Jasmin E Washington
    Department of Astronomy, University of Virginia, Charlottesville, VA 22904, USA
  • Laura M Fissel
    National Radio Astronomy Observatory, Charlottesville, VA 22904, USA
  • Rachel K Friesen
    National Radio Astronomy Observatory, Charlottesville, VA 22904, USA
  • Zhi-Yun Li
    Department of Astronomy, University of Virginia, Charlottesville, VA 22904, USA
  • Jaime E Pineda
    Max-Planck-Institut für extraterrestrische Physik, Giessenbachstrasse 1, D-85748 Garching, Germany
  • Adam Ginsburg
    Department of Astronomy, University of Florida, Gainesville, FL 32611, USA
  • Helen Kirk
    Herzberg Astronomy and Astrophysics, National Research Council of Canada, Victoria, BC V9E 2E7, Canada
  • Samantha Scibelli
    Department of Astronomy, University of Arizona, Tucson, AZ 85721, USA
  • Felipe Alves
    Max-Planck-Institut für extraterrestrische Physik, Giessenbachstrasse 1, D-85748 Garching, Germany
  • Elena Redaelli
    Max-Planck-Institut für extraterrestrische Physik, Giessenbachstrasse 1, D-85748 Garching, Germany
  • Paola Caselli
    Max-Planck-Institut für extraterrestrische Physik, Giessenbachstrasse 1, D-85748 Garching, Germany
  • Anna Punanova
    Ural Federal University, Mira St 19, Yekaterinburg 620002, Russia
  • James Di Francesco
    Herzberg Astronomy and Astrophysics, National Research Council of Canada, Victoria, BC V9E 2E7, Canada
  • Erik Rosolowsky
    Department of Physics, University of Alberta, Edmonton, AB T6G 2E1, Canada
  • Stella S R Offner
    Department of Astronomy, University of Texas at Austin, Austin, TX 78712, USA
  • Peter G Martin
    Canadian Institute for Theoretical Astrophysics, University of Toronto, Toronto, ON M5S 3H8, Canada
  • Ana Chacón-Tanarro
    Observatorio Astronómico Nacional (OAN-IGN), Alfonso XII 3, E-28014 Madrid, Spain
  • Hope H-H Chen
    Department of Astronomy, University of Texas at Austin, Austin, TX 78712, USA
  • Michael C-Y Chen
    Department of Physics, University of Alberta, Edmonton, AB T6G 2E1, Canada
  • Jared Keown
    Department of Physics, University of Alberta, Edmonton, AB T6G 2E1, Canada
  • Youngmin Seo
    Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA
  • Yancy Shirley
    Department of Astronomy, University of Arizona, Tucson, AZ 85721, USA
  • Hector G Arce
    Department of Astronomy, Yale University, New Haven, CT 06520, USA
  • Alyssa A Goodman
    Harvard–Smithsonian Center for Astrophysics, Cambridge, MA 02138, USA
  • Christopher D Matzner
    Department of Astronomy & Astrophysics, University of Toronto, Toronto, ON M5S 3H4, Canada
  • Philip C Myers
    Harvard–Smithsonian Center for Astrophysics, Cambridge, MA 02138, USA
  • 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>

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