Fe II transition probabilities and the solar iron abundance

Details Fe II transition probabilities and the solar iron abundance Fe II transition probabilities and the solar iron abundance

May 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990a%26a...231..536p&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 231, no. 2, May 1990, p. 536-542. Research supported by SNSF.

Astronomy and Astrophysics

Astrophysics

36

Abundance, Iron, Metallicity, Near Infrared Radiation, Solar Spectra, Nonequilibrium Thermodynamics, Photosphere, Thermodynamic Equilibrium, Transition Probabilities

Scientific paper

Branching fractions for three near-infrared Fe II lines are presented that fulfill the requirements necessary for an accurate solar abundance determination. The lines belong to the dominant ionization stage and are weak enough to lie on the linear part of the curve of growth. The resulting abundance is insensitive to deviations from local thermodynamic equilibrium and is independent of assumptions concerning the temperature model and line-broadening parameters. From the transition probabilities and from accurate solar equivalent widths, a solar photospheric iron abundance is obtained.

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