Opacity and Atmospheric Structure at the Solar Limb

Details Opacity and Atmospheric Structure at the Solar Limb Opacity and Atmospheric Structure at the Solar Limb

Oct 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999esasp.446..321f&link_type=abstract

8th SOHO Workshop: Plasma Dynamics and Diagnostics in the Solar Transition Region and Corona. Proceedings of the Conference hel

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Although solar EUV emission is dominated by inhomogeneities, it seems observed opacities may be reasonably well modelled using simple atmosphere models in conjunction with escape probability techniques. The latter avoid the need for a full solution to the radiative transfer equation. In the work presented here we demonstrate the effectiveness of such models in describing the quiet sun opacity variation as observed by SUMER, in spectral lines of CII and CIII on crossing the solar limb. We consider contrasting atmosphere models and include the effects of instrumentally scattered light.

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