Physical properties of the solar chromosphere deduced from optically thick lines. I - Observations, data reduction, and modelling of an average plage

Details Physical properties of the solar chromosphere deduced from optically thick lines. I - Observations, data reduction, and modelling of an average plage Physical properties of the solar chromosphere deduced from optically thick lines. I - Observations, data reduction, and modelling of an average plage

Nov 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981a%26a...103..160l&link_type=abstract

Astronomy and Astrophysics, vol. 103, no. 1, Nov. 1981, p. 160-176. Centre National d'Etudes Spatiales

Astronomy and Astrophysics

Astrophysics

50

Chromosphere, Faculae, Line Spectra, Solar Spectra, Data Processing, H Lines, Mathematical Models, Optical Thickness, Oso-8, Physical Properties, Solar Atmosphere

Scientific paper

Simultaneous Ca II H and K, Mg II h and k, and H I Lyman-alpha and Lyman-beta profiles have been recorded by the OSO-8/LPSP spectrometer on a quiet sun area and a part of plage, McMath 13738. After data reduction and filtering, a full set of calibrated profiles is obtained. Using a code developed at LPSP (Gouttebroze et al., 1978), profiles computed from VAL III model C (Vernazza et al., 1981) are compared to observations. A specific plage model has been computed to fit the observed profiles. This model reproduces successfully Ca II H and K, and H I Lyman-alpha and Lyman-beta, but partly fails with Mg II h and k. Atmospheric inhomogeneities and dynamical effects may contribute to this discrepancy, and it is proposed that the level number entering in the Mg II computation be increased to take account of a likely fluorescence induced by the H I Lyman-beta radiation field.

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