34th Solar Physics Division Meeting, June 2003
Session 3 Data Analysis Challenges II
Poster, Monday, June 16, 2003, 3:30-5:00pm, Mezzanine

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[3.01] Physical Modeling of the Solar Radiation, Current Status and Prospects

J.M. Fontenla (LASP, University of Colorado Boulder), E.H. Avrett (CFA, Harvard-Smithsonian Institution), M. Goodman (ISR, Fairmont, WV), O.W. White, G. Rottman (LASP, University of Colorado Boulder), P. Fox (HAO, Boulder), J. Harder (LASP, University of Colorado Boulder)

Physical models that include full NLTE radiative transfer as well as particle transport and MHD processes are the key to understanding the solar radiative output and also are essential to our understanding of heating and the dynamics of the solar atmosphere, in particular for chromospheric layers. SOHO observations show that chromospheric emission lines do not vary dramatically in time and that chromospheric heating, even in the quiet Sun, is not simply due to, p-modes induced, strong shock waves passing through the chromosphere. The physics of the chromospheric heating is more complicated and remains elusive. The chromospheric and coronal heating are likely closely related to the dynamics in these regions as well as in the thin chromosphere-corona transition region since they are a coupled system. Solar atmospheric heating and dynamics are strongly affected by the magnetic fields and MHD mechanisms must be considered. Models for the upper photosphere and chromosphere should also consider NLTE radiative transfer and radiative losses as well as particle transport processes including tensor electric resistivity with magnetic field. Models for the transition region and coronal layers must also consider particle diffusion. In this paper we show schematically: 1) the current state of our research on modeling observed features of the solar structure and their radiative signatures; 2) the application of this modeling to the Earth solar irradiance and comparisons with observations; 3) the key achievements and the needed improvements of the modeling; 4) our plans for future research starting from ab initio semi-empirical models based on observations, and, while maintaining the agreement with relevant observations, moving towards physically consistent models that include key MHD processes thereby replacing empirical constraints by physically consistent processes and boundary conditions.


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Bulletin of the American Astronomical Society, 35 #3
© 2003. The American Astronomical Soceity.