Coronal heating by magnetohydrodynamic turbulence driven by reflected low-frequency waves

A candidate mechanism for the heating of the solar corona in open field line regions is described. The interaction of Alfven 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 Alfven timescales. A phenomenology is presented, providing estimates of achievable heating efficiency that are most favorable.