Non-LTE analysis of neutral magnesium in the solar atmosphere

Details Non-LTE analysis of neutral magnesium in the solar atmosphere Non-LTE analysis of neutral magnesium in the solar atmosphere

May 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998a%26a...333..219z&link_type=abstract

Astronomy and Astrophysics, v.333, p.219-230 (1998)

Astronomy and Astrophysics

Astrophysics

39

Atomic Processes, Line: Formation, Sun: Abundances, Sun: Photosphere

Scientific paper

We investigate the formation of neutral magnesium lines in the solar photosphere with an atomic model containing 83 levels plus the ground state of Mg ii connected via radiative and collisional interactions. Synthetic line flux and intensity profiles are compared with the solar spectrum to study the relevant physical processes and their influence on the level populations and line profiles. For neutral magnesium with the photoionization edges of its three lowest states at lambda lambda 1620, 2514 and 3757 Angstroms the reduction of the ultraviolet radiation field due to metallic line absorption has been taken into account using Kurucz' (\cite{KURUCZ92}) ODF opacities. In the photosphere of a cool star excitation and ionization due to collisions with neutral hydrogen can outweigh electron collisions. Therefore the influence of different types of collisional interactions with electrons and neutral hydrogen atoms is examined. General agreement with solar line profiles in the visible and infrared is found for an atomic model with both electron collisions and strongly reduced but significantly large neutral hydrogen collision rates. Our investigation thus extends previous results to lines of all different excitation energies. The atomic model found from the analysis of the solar spectrum will serve as a reference for the investigation of cool metal-poor stars in which both the reduced electron collision rates and the enhanced UV intensities lead us to expect more pronounced deviations from LTE.

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