Abstract
Diffusive shock acceleration is the theory of particle acceleration through multiple shock crossings. In order for this process to proceed at a rate that can be reconciled with observations of high-energy electrons in the vicinity of the shock, and for cosmic rays protons to be accelerated to energies up to observed galactic values, significant magnetic field amplification is required. In this review we will discuss various theories on how magnetic field amplification can proceed in the presence of a cosmic ray population. On both short and long length scales, cosmic ray streaming can induce instabilities that act to amplify the magnetic field. Developments in this area that have occurred over the past decade are the main focus of this paper.
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Acknowledgements
We would like to acknowledge ISSI for their support during, and the organisation of, the workshop on particle acceleration in cosmic plasmas. K.M.S. and A.R.B. acknowledge support from the UK Science Technology and Facilities Council grant ST/H001948/1; and from the European Research Council under the European Community’s Seventh Framework Programma (FP7/2007-2013)/ERC grant agreement no. 247039. A.M.B. was supported in part by the RAS Programs, by the RFBR grant 11-02-12082-ofi-m-2011, and also by the Russian government grant 11.G34.31.0001 to the Saint-Petersburg State Politechnical University.
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Schure, K.M., Bell, A.R., O’C Drury, L. et al. Diffusive Shock Acceleration and Magnetic Field Amplification. Space Sci Rev 173, 491–519 (2012). https://doi.org/10.1007/s11214-012-9871-7
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DOI: https://doi.org/10.1007/s11214-012-9871-7