On the variation of solar flare coronal X-ray source sizes with energy

Jeffrey, N. L.S. , Kontar, E. P. , Bian, N. H. and Emslie, A. G. (2014) On the variation of solar flare coronal X-ray source sizes with energy. Astrophysical Journal, 787(1), 86. (doi:10.1088/0004-637X/787/1/86)

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Observations with RHESSI have enabled the detailed study of the structure of dense hard X-ray coronal sources in solar flares. The variation of source extent with electron energy has been discussed in the context of streaming of non-thermal particles in a one-dimensional cold target model and the results used to constrain both the physical extent of, and density within, the electron acceleration region. Here, we extend this investigation to a more physically realistic model of electron transport that takes into account the finite temperature of the ambient plasma, the initial pitch angle distribution of the accelerated electrons, and the effects of collisional pitch angle scattering. The finite temperature results in the thermal diffusion of electrons, which leads to the observationally inferred value of the acceleration region volume being an overestimate of its true value. The different directions of the electron trajectories, a consequence of both the non-zero injection pitch angle and scattering within the target, cause the projected propagation distance parallel to the guiding magnetic field to be reduced, so that a one-dimensional interpretation can overestimate the actual density by a factor of up to ~6. The implications of these results for the determination of acceleration region properties (specific acceleration rate, filling factor, etc.) are discussed.

Item Type:Articles
Glasgow Author(s) Enlighten ID:Kontar, Dr Eduard and Jeffrey, Dr Natasha and Bian, Dr Nicolas Horace
Authors: Jeffrey, N. L.S., Kontar, E. P., Bian, N. H., and Emslie, A. G.
College/School:College of Science and Engineering > School of Physics and Astronomy
Journal Name:Astrophysical Journal
Publisher:Institute of Physics Publishing, Inc.
ISSN (Online):1538-4357
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