Iron abundance derived from two-dimensional inhomogeneous solar model atmospheres. Fe I and Fe II lines (center of the disk).

Details Iron abundance derived from two-dimensional inhomogeneous solar model atmospheres. Fe I and Fe II lines (center of the disk). Iron abundance derived from two-dimensional inhomogeneous solar model atmospheres. Fe I and Fe II lines (center of the disk).

Jan 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996kpcb...12...13g&link_type=abstract

Kinematics Phys. Celest. Bodies, Vol. 12, No. 4, p. 13 - 20

Physics

1

Line Profiles: Solar Models, Line Profiles: Solar Photosphere, Solar Spectrum: Iron

Scientific paper

Two-dimensional hydrodynamic solar model atmospheres are used to determine the iron abundance in the solar photosphere by fitting calculated equivalent widths and central depths of Fe I and Fe II lines to observed ones. The effect of atmospheric inhomogeneities is found to give rise to uncertainties in the iron abundance of about 0.1 dex for weak Fe I lines with low excitation potentials and 0.05 dex for weak Fe II lines. A self-consistent velocity field in 2-D models with a statistically wide spectrum of inhomogeneities would suffice to reproduce observed line profiles.

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