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Galactic magnetic fields and their interactions with the gas and cosmic rays

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Abstract

(i) The controversy of dynamo or primordial origin of galactic magnetic fields is summarized and extended to show that the dynamo theory appears to fail. However, much more important than their origin are the characteristics of the fields and their interactions with the gas and cosmic rays. (ii) A passive magnetic field frozen into a turbulent plasma is not dissipated like a cloud of smoke (‘turbulent or eddy diffusion’) as believed previously. On the contrary it is amplified exponentially until, within a few eddy periods, either the growing magnetic stresses halt the turbulence or the field becomes chaotic. Even if the Petschek reconnection mechanism operates, the field is always disordered to a scale <0.1L, whereL is the eddy dimension. The investigation may at last provide a semi-quantitative deductive theory of hydromagnetic eddies. (iii) It is concluded that the gas motions observed in our Galaxy are not convective but are mainly hydromagnetic waves or oscillations, with the magnetic field in control. The significance of this result is discussed in connection with the overall gas velocity field, the creation of stars and stellar systems, and with the origin and distribution of cosmic rays.

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  1. CSIRO National Measurement Laboratory, Sydney, Australia

    J. H. Piddington

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  1. J. H. Piddington
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Piddington, J.H. Galactic magnetic fields and their interactions with the gas and cosmic rays. Astrophys Space Sci 37, 183–196 (1975). https://doi.org/10.1007/BF00646072

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