MHD Wave Turbulence as the Energy and Momentum Source for Heating the Solar Corona and Driving the Solar Wind in Global Space Weather Models

Details MHD Wave Turbulence as the Energy and Momentum Source for Heating the Solar Corona and Driving the Solar Wind in Global Space Weather Models MHD Wave Turbulence as the Energy and Momentum Source for Heating the Solar Corona and Driving the Solar Wind in Global Space Weather Models

Dec 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufmsh43a1936s&link_type=abstract

American Geophysical Union, Fall Meeting 2011, abstract #SH43A-1936

Physics

Plasma Physics

[7509] Solar Physics, Astrophysics, And Astronomy / Corona, [7549] Solar Physics, Astrophysics, And Astronomy / Ultraviolet Emissions, [7863] Space Plasma Physics / Turbulence

Scientific paper

Recent Hinode observations upped the estimates for the energy associated with Alfven waves generated in the solar chromosphere. This energy has been found to be sufficient to heat the solar corona and to explain the solar wind acceleration and heating. At present time, many physical models for the coronal heating, the solar wind, as well as the energetic particle acceleration and transport, incorporate the MHD wave turbulence. This paper presents a new model for coronal heating which adopts MHD wave turbulence as the dominant energy for heating the solar corona and driving the solar wind. We re-formulate an empirical model for the coronal heating in terms of the dissipation length controlling the wave damping. The model for the solar corona is validated against EUV observations from the EIT instrument on-board SOHO.

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