Coronal heating by quasi-2D MHD turbulence driven by non-WKB wave reflection

Details Coronal heating by quasi-2D MHD turbulence driven by non-WKB wave reflection Coronal heating by quasi-2D MHD turbulence driven by non-WKB wave reflection

Jun 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999aipc..471..361m&link_type=abstract

The solar wind nine conference. AIP Conference Proceedings, Volume 471, pp. 361-364 (1999).

Physics

1

Magnetohydrodynamics And Plasmas

Scientific paper

We present a candidate mechanism for heating of the solar corona, via the interaction of (chromospherically-generated) Alfvén waves, their reflections, and quasi-two dimensional (relative to the mean magnetic field) MHD turbulence. The non-propagating nature of the latter means that the restrictive Alfvén timescale constraints associated with high frequency wave heating models are avoided. A phenomenology for this mechanism is described here, and ``proof of concept'' support from reduced MHD (RHMD) simulations is also discussed. Estimates of the achievable heating efficiency based on turbulence models are favorable, and encourage further investigation of the model's quantitative feasibility.

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