Astronomy and Astrophysics – Astrophysics
Scientific paper
Sep 1983
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983apj...272..723r&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 272, Sept. 15, 1983, p. 723-738.
Astronomy and Astrophysics
Astrophysics
17
H Lines, Lyman Alpha Radiation, Solar Spectra, Spectral Energy Distribution, Atomic Collisions, Chromosphere, Radiative Transfer, Solar Temperature, Spectral Line Width, Thermalization (Energy Absorption)
Scientific paper
A form for the Lyman-alpha redistribution function that is modified to include the effects of collisional coupling between different energy states is presented. It is noted that this extends the work of Yelnik et al. (1981) and Roussel-Dupre(1982). By separating the source function into its primary components at all heights, the formation of Lyman-alpha radiation is investigated in detail. Frequencies in the line wing can be mapped back in such a way that the heights of formation for a change in lambda of plus or minus 0.5-6 A span the entire solar chromosphere. The usefulness of the Lyman-alpha wing as an atmospheric probe, however, is limited by long thermalization lengths, which result from almost coherent scattering outside of the Doppler core. When the line profiles calculated from the chromospheric models of Vernazza et al. (1981) are compared with the quiet-sun observations of Roussel-Dupre, agreement is found in integrated core intensities and in the line wing shape and normalized center-to-limb behavior. The calculated wing intensities, however, are a factor of four too small.
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