The formation of the MG I emission features near 12 microns

Details The formation of the MG I emission features near 12 microns The formation of the MG I emission features near 12 microns

Jan 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992a%26a...253..567c&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 253, no. 2, Jan. 1992, p. 567-585. Research supported by Utrecht State Univers

Astronomy and Astrophysics

Astrophysics

91

Chromosphere, Magnesium, Metallicity, Solar Atmosphere, Solar Spectra, Line Spectra, Solar Radio Emission

Scientific paper

The formation of two Mg I 12-micron emission features in the solar spectrum, the existence of which was reported by Murcray et al. (1981), is explained using plane-parallel nonlocal thermodynamic equilibrium modeling with a radiative-equilibrium model atmosphere without chromosphere. It is shown that these emissions are a natural consequence of population depletion by line photon losses followed by population replenishment from the ionic reservoir in the highly excited levels. The results confirm the suggestion by Lemke and Holweger (1987) that the 12-micron lines are formed in the photosphere and disprove the claim by Zirin and Popp (1989) that the temperature minimum occurs much deeper than in standard models of the solar atmosphere.

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