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Heating and dynamics of the quiet solar chromosphere

Published online by Cambridge University Press:  01 September 2007

Wolfgang Kalkofen
Wolfgang Kalkofen*
Affiliation:
Harvard-Smithsonian Center for Astrophysics email: wkalkofen@cfa.harvard.edu
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Abstract

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The quiet solar chromosphere in regions with negligible magnetic field is believed to be heated by acoustic waves. But their energy flux, measured in the upper photosphere with the Transition Region And Coronal Explorer (TRACE), has been found to be insufficient to account for the radiative emission from the chromosphere. Wedemeyer-Böhm et al. (2007) and Cuntz et al. (2007), employing a 3D hydrodynamical model by Wedemeyer et al. (2004), have proposed that the spatial resolution of TRACE is inadequate to resolve intensity fluctuations that occur on small spatial scales. This paper accepts the principle of spatial averaging by TRACE as a qualitative explanation for the low acoustic flux but finds that the hydrodynamical model is too much simplified in the treatment of radiative energy exchange to provide a quantitative measure of the suppression of the fluctuations. The heating mechanism of the chromosphere thus remains an open question.

Keywords

waveshydrodynamicsradiative transferSun: atmosphereSun: photosphereSun: chromosphere
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 3 , Symposium S247: Waves & Oscillations in the Solar Atmosphere: Heating and Magneto-Seismology , September 2007 , pp. 93 - 98
Copyright
Copyright © International Astronomical Union 2008

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