Abstract
Our ability to test aspects of solar flare energy transport models hinges on our adequately characterizing the SXR-emitting plasma’s motions. In particular, to test the electron beam model of energy transport, we must obtain an accurate representation of the plasma’s velocity distribution, and thereby momentum, contemporaneously with profiles of the HXR flux and spectrum.
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Newton, E.K., A.G. Emslie, & J.T. Mariska 1995, ApJ, 447, 915.
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© 1996 Kluwer Academic Publishers
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Newton, E.K., Emslie, A.G., Mariska, J.T. (1996). Dynamical Response of the Solar Atmosphere to Flare Heating. In: Uchida, Y., Kosugi, T., Hudson, H.S. (eds) Magnetodynamic Phenomena in the Solar Atmosphere. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-0315-9_138
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DOI: https://doi.org/10.1007/978-94-009-0315-9_138
Publisher Name: Springer, Dordrecht
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