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Date and Time of the Query: 2019-06-26 T06:21:53 PDT
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For refcode 1989A&A...213...19K:
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Copyright by European Southern Observatory (ESO). Reproduced by permission
1989A&A...213...19K Configuration of large-scale magnetic fields in spiral galaxies Y. Krasheninnikova (Baryshnikova), A. Ruzmaikin, D. Sokoloff, and A. Shukurov Space Research Institute, Academy of Sciences, Profsoyusnaya ul. 84/32, Moscow 117810, USSR Institute of Terrestrial Magnetism, Ionosphere and Radiowave Propagation, Academy of Sciences, Troitsk 142092, Moscow Region, USSR Physics Department, Moscow State University, Lenin Hills, Moscow 119899, USSR Received May 16, accepted August 30, 1988 Summary. Within the framework of the thin-disc galactic dynamo model of Baryshnikova et al. (1987), magnetic lines for the axisymmetric m = 0 and non-axisymmetric m = 1 dynamo modes are presented. The calculated pitch angles of magnetic lines in the galaxies M31, M51, M81, IC 342 and the Milky Way agree with observational data. Spatial distributions of the Faraday rotation measures produced by axisymmetric and non-axisymmetric fields and their superpositions are discussed. Effective generation of the m = 1 dynamo mode in M81 is shown. Distribution of magnetic field in IC 342 is discussed in detail. It is shown that measurements of pitch angles of magnetic lines in outer parts of galaxies can be used for estimation of the ratio of the energy-range scale of interstellar turbulence to the thickness of the ionized gaseous disc. We discuss possible reasons of presence of bisymmetric fields among the observed magnetic structures. Non-axisymmetric distortions of the galactic disc with azimuthal wave number one result in two effects first, the basic dynamo mode, remaining axisymmetric at small galactocentric distances, acquires a m = 1 correction in the outer part of the disc. Second, the difference between the growth rates of the m = 0 and m = 1 dynamo modes considerably decreases In contrast, weak perturbations from spiral arms do not affect growth rates of bisymetric dynamo modes Additional generation of the azimuthal field by helical turbulence ({alpha}^2^-dynamo) cannot make non-axisymmetric modes prevalent in a thin disc. Key words: spiral galaxies - interstellar medium - large-scale magnetic fields - turbulent dynamos
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