A non-LTE study of the solar emission lines near 12 microns

Astronomy and Astrophysics – Astrophysics

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Emission Spectra, Far Infrared Radiation, Line Shape, Nonequilibrium Thermodynamics, Solar Atmosphere, Solar Spectra, Aluminum, Magnesium

Scientific paper

The formation of the peculiar FIR emission lines in the solar spectrum, identified by Chang and Noyes (1983) as transitions between highly excited states of Mg I and Al I, is investigated. The statistical equilibrium of Mg I and the influence of various input data on the line profile are studied. An emission core is not easily generated. The chromospheric contribution to these rather faint lines turns out to be negligible unless it is assumed ad hoc that the line source function exceeds the non-LTE prediction by a large factor. An alternative requiring less severe assumptions is pointed out. In this scheme the emission is purely photospheric. Disk-center and limb profiles of Mg I (818.058/cm) can be reproduced by postulating that a slight overexcitation prevails in the upper photosphere, with log tau(5000) = about -2, in the sense that the population ratio of upper to lower level exceeds the LTE value by a few percent.

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