Heating of the solar corona by Alfven waves - self-induced opacity
Abstract
Static distributions of temperature and wind velocity at the transition region are calculated within the framework of magnetohydrodynamics (MHD) of completely ionized hydrogen plasma. The numerical solution of the derived equations gives the width of the transition layer between the chromosphere and the corona as a self-induced opacity of high-frequency Alfven waves (AW). The domain wall is direct consequence of the self-consistent MHD treatment of AW propagation. The low-frequency MHD waves coming from the Sun are strongly reflected by the narrow transition layer, while the high-frequency waves are absorbed - that is why we predict considerable spectral density of the AW in the photosphere. The numerical method allows consideration of incoming AW with arbitrary spectral density. The idea that Alfven waves might heat the solar corona belongs to Alfven, we simply solved the corresponding MHD equations. The comparison of the solution to the experiment is crucial for revealing the heating mechanism.
Keywords
Cite
@article{arxiv.1103.2233,
title = {Heating of the solar corona by Alfven waves - self-induced opacity},
author = {Todor M. Mishonov and Nedeltcho I. Zahariev and Rositsa V. Topchiyska and Boian V. Lazov and Stefan B. Mladenov and Albert M. Varonov},
journal= {arXiv preprint arXiv:1103.2233},
year = {2016}
}
Comments
11 pages, 8 figures; v3: illustrative numerical solutions of the derived equations, new figures added, discussion of magnetic Prandtl number added; v4: typos corrected and references added