Abstract
ALTHOUGH there are various methods of investigating experimentally the integral properties of galactic magnetic fields (see, for example, ref. 1), little is known experimentally of the nature of the random component of these fields, at least as far as structures with characteristic lengths ≲ 1 pc are concerned. Here I shall describe a method which, supposing the diffusion approximation of cosmic-ray propagation to be valid, is suitable for determining the structural composition of random galactic fields on the basis of cosmic-ray measurements, down to structures with characteristic lengths ∼ 0.001–1 pc.
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SOMOGYI, A. Structure of irregular galactic magnetic fields. Nature 255, 689–690 (1975). https://doi.org/10.1038/255689a0
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DOI: https://doi.org/10.1038/255689a0
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