Abstract
Predictions of solar flux and limb darkening calculated from the Utrecht Reference Model, the Mutschlecner model, and the Bilderberg Continuum Atmosphere are compared with the rocket ultraviolet observations. The calculations employ recent experimental and theoretical determinations of metallic photo-ionization cross-sections. The spectral region between the continuous absorption edge from the first excited level of silicon at 1680 Å and the ground-state absorption edge at 1525 Å proves particularly significant for an investigation of the solar temperature minimum. The analysis indicates that the solar temperature minimum is relatively broad and flat, having a nearly constant temperature over somewhat more than a scale height, and that the chromospheric rise occurs just above τ5000 = 10−4 or so. Within the assumptions of the present models, a satisfactory interpretation of the ultraviolet spectrum can be reached with a temperature minimum of 4600° ± 100 °K.
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Gingerich, O., Rich, J.C. (1968). The Far Ultraviolet Spectrum of the Sun. In: de Jager, C. (eds) The Structure of the Quiet Photosphere and the Low Chromosphere. Springer, Dordrecht. https://doi.org/10.1007/978-94-010-3470-8_8
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DOI: https://doi.org/10.1007/978-94-010-3470-8_8
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