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A candidate mechanism for the heating of the solar corona in open field line regions is described. The interaction of Alfve n waves, generated in the photosphere or chromosphere, with their reflections and the subsequent driving of quasi-two-dimensional MHD turbulence is considered. A nonlinear cascade drives fluctuations toward short wavelengths which are transverse to the mean field, thereby heating at rates insensitive to restrictive Alfve n timescales. A phenomenology is presented, providing estimates of achievable heating efficiency that are most favorable.
Matthaeus et al. (Mon,) studied this question.