Iron abundance derived from two-dimensional inhomogeneous solar model atmospheres. Fe I and Fe II lines (center of the disk).
Abstract
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.
- Publication:
-
Kinematics and Physics of Celestial Bodies
- Pub Date:
- January 1996
- Bibcode:
- 1996KPCB...12d..13G
- Keywords:
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- Line Profiles: Solar Models;
- Line Profiles: Solar Photosphere;
- Solar Spectrum: Iron