Magnetic fields from filaments to cores

P. M. Koch, Y. W. Tang, N. L. Chapman, A. Duarte-Cabral, P. T.P. Ho, Giles A Novak, N. Peretto, Y. N. Su, S. Takakuwa, H. W. Yen

Research output: Contribution to journalConference article

Abstract

How important is the magnetic (B-) field when compared to gravity and turbulence in the star-formation process? Does its importance depend on scale and location? We summarize submm dust polarization observations towards the large filamentary infrared dark cloud G34 and towards a dense core in the high-mass star-forming region W51. We detect B-field orientations that are either perpendicular or parallel to the G34 filament axis. These B-field orientations further correlate with local velocity gradients. Towards three cores in G34 we find a varying importance between B-field, gravity, and turbulence that seems to dictate varying types of fragmentation. At highest resolution towards the gravity-dominated collapsing core W51 e2 we resolve new B-field features, such as converging B-field lines and possibly magnetic channels.

Original languageEnglish (US)
Pages (from-to)557-559
Number of pages3
JournalMemorie della Societa Astronomica Italiana - Journal of the Italian Astronomical Society
Volume88
Issue number4
StatePublished - Jan 1 2017
Event2017 Conference Francesco's Legacy: Star Formation in Space and Time - Firenze, Italy
Duration: Jun 5 2017Jun 9 2017

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Keywords

  • ISM: Individual objects: (G34,W51)
  • ISM: Magnetic field
  • Polarization

ASJC Scopus subject areas

  • Electrical and Electronic Engineering
  • Radiology Nuclear Medicine and imaging
  • Astronomy and Astrophysics
  • Instrumentation
  • Atomic and Molecular Physics, and Optics

Cite this

Koch, P. M., Tang, Y. W., Chapman, N. L., Duarte-Cabral, A., Ho, P. T. P., Novak, G. A., Peretto, N., Su, Y. N., Takakuwa, S., & Yen, H. W. (2017). Magnetic fields from filaments to cores. Memorie della Societa Astronomica Italiana - Journal of the Italian Astronomical Society, 88(4), 557-559.