Empirical Models of the Extended Solar Corona

Details Empirical Models of the Extended Solar Corona Empirical Models of the Extended Solar Corona

May 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997spd....28.0303k&link_type=abstract

American Astronomical Society, SPD meeting #28, #03.03; Bulletin of the American Astronomical Society, Vol. 29, p.907

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Scientific paper

Ultraviolet spectroscopy is being used to produce self consistent empirical models of polar coronal holes and equatorial streamers in the extended solar corona. The models are intended to provide experimental values for many of the primary plasma parameters of the extended corona, which can then be used to constrain theoretical coronal and solar wind models. The empirical models are based on synoptic observations and other measurements of spectral line profiles and intensities of H I Lyalpha , O VI 1032 Angstroms and 1037 Angstroms, Fe XII 1242 Angstroms, Mg X 625 Angstroms and several others. Information about velocity distributions, outflow velocities, densities and elemental abundances as derived from the observations are specified in the models. The models used to specify the empirically derived parameters include a description of well established theoretical processes such as those controlling ionization balance, collisional excitation, and resonant scattering. They do not include any descriptions of less well established processes such as heating functions, transverse wave motions or direct momentum deposition by waves. The intent is to provide, to the maximum extent possible, empirical descriptions that can be used, together with theoretical models, to help identify the dominant physical processes responsible for coronal heating, solar wind acceleration and the chemical composition of the solar wind. This work is supported by NASA Grant NAG5-3192 to the Smithsonian Astrophysical Observatory, the Italian Space Agency and Swiss funding sources.

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