Broadening and shift of Fe I lines perturbed by atomic hydrogen

Details Broadening and shift of Fe I lines perturbed by atomic hydrogen Broadening and shift of Fe I lines perturbed by atomic hydrogen

Sep 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987soph..112..227g&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 112, no. 2, 1987, p. 227-232.

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Hydrogen Atoms, Ion Atom Interactions, Iron, Photosphere, Solar Spectra, Spectral Line Width, Computational Astrophysics, Solar Temperature

Scientific paper

The atomic potentials of Hindmarsh et al. (1967, 1970) are used to compute the values of the damping and shift for a number of Fe I lines produced by neutral hydrogen perturbers at temperatures typical of the solar photosphere. It is found that the rms radius and the effective radius of the radiating atom (which determine the force constants in the interatomic potential) can be simply related to each other, depending on the orbital quantum number of the atomic level. The present values for the pressure shift of the Fe I lines confirm the previous finding that the pressure shift for the Fe I lines is negligible with respect to the convective blueshift produced by the solar granulation.

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