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Date and Time of the Query: 2019-06-19 T13:44:30 PDT
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For refcode 1992A&A...255..100V:
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Copyright by European Southern Observatory (ESO). Reproduced by permission
1992A&A...255..100V Research Note On the quadrisymmetric (m = 2) magnetic fields in spiral galaxies J. P. Vallee JCMT Group, Herzberg Institute of Astrophysics, National Research Council of Canada, 100 Sussex Drive, Ottawa, Ontario K1A 0R6, Canada JCMT Unit, Royal Observatory, Blackford Hill, Edinburgh, Scotland EH9 3HJ, UK Received April 3, accepted August 26, 1991 Abstract. The large scale magnetic field structures of spiral galaxies have been observed to consist of either the simple m_azim_ = 0 axisymmetric azimuthal magnetic fields, or the simple m_azim_ = 1 bisymmetric azimuthal magnetic fields, or has "neither" field structure (considerable complexity, Beck 1991). Where should one look for the m_azim_= 2 mode? I show that the observations so far (m_azim_ = 0 and M_HI_ = large; m_azim_ = 1 and M_HI_ = average) suggest an empirical induction (m_azim_ = 2 and M_HI_ = small). Also, the theories so far (possible m_azim_ mode being inversely proportional to the ionised Hydrogen scale height, and thus to the HI gas scale height) suggest a progressive elimination (m_azim_ = 2 has never been predicted in galaxies with M_HI_ = average or large). M_HI_ is the neutral hydrogen mass. Here I predict that the m_azim_ = 2 quadrupolar azimuthal magnetic field in a spiral galaxy (if detected) will be associated with a small neutral hydrogen gas mass M_HI_. I also review the available data on star formation efficiency versus large-scale magnetic fields in galaxies. High values of the star formation efficiency cannot be used to predict accurately the large-scale magnetic fields. Key words: spiral galaxies - interstellar magnetic field - turbulent dynamo - H I radio line - Faraday polarization
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