Computer Science
Scientific paper
Sep 1971
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1971saosr.338.....c&link_type=abstract
SAO Special Report #338 (1971)
Computer Science
10
Scientific paper
We have made a detailed study of the formation of the strongest ultraviolet emission lines of Mg II, O I, C II, and C III in the solar atmosphere. We solve the equations of statistical equilibrium and radiative transfer for each ion, using a general computer program that is capable of solving non-LTE line-formation problems for arbitrary atmospheric and atomic models. Interpreting the results in terms of the structure of the solar atmosphere, we conclude that the HSRA atmosphere has a temperature too low by about 500 K near H = 1100 km and that a temperature plateau with Te ≍ 18,000 K and width close to 60 km exists in the upper chromosphere. We also investigate the structure of the solar atmosphere in the range 2 20,000 to 100,000 K and the effects of microturbulence on the formation of lines. We solve some approximate analytic line-formation problems relevant to the more exact solutions derived later. In the Appendix we attempt to make the best possible fit to the Ca II K line center-to-limb profiles with a one-component atmosphere, with an assumed source function and microturbulent velocity.
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