Pitch-angle diffusion and Bohm-type approximations in diffusive shock acceleration
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Date
2019-02-27
Authors
Riordan, John Daniel
Pe’er, Asaf
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IOP Publishing on behalf of the American Astronomical Society
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Abstract
The problem of accelerating cosmic rays is one of fundamental importance, particularly given the uncertainty in the conditions inside the acceleration sites. Here we examine diffusive shock acceleration in arbitrary turbulent magnetic fields, constructing a new model that is capable of bridging the gap between the very weak (δB/B 0 Lt 1) and the strong turbulence regimes. To describe the diffusion we provide a quantitative analytical description of the "Bohm exponent" in each regime. We show that our results converge to the well known quasi-linear theory in the weak turbulence regime. In the strong regime, we quantify the limitations of the Bohm-type models. Furthermore, our results account for the anomalous diffusive behavior which has been noted previously. Finally, we discuss the implications of our model in the study of possible acceleration sites in different astronomical objects.
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Keywords
Acceleration of particles , Cosmic rays , Methods: numerical , Scattering , Turbulence
Citation
Riordan, J. D. and Pe’er, A. (2019) ‘Pitch-angle diffusion and Bohm-type approximations in diffusive shock acceleration’, Astrophysical Journal, 873(1), 13 (12pp). doi: 10.3847/1538-4357/aaffd2
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© 2019, American Astronomical Society. All rights reserved.