A Technique for the Study of Stellar Convection: The Visible Solar Flux Spectrum

Details A Technique for the Study of Stellar Convection: The Visible Solar Flux Spectrum A Technique for the Study of Stellar Convection: The Visible Solar Flux Spectrum

Sep 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999pasp..111.1132h&link_type=abstract

The Publications of the Astronomical Society of the Pacific, Volume 111, Issue 763, pp. 1132-1143.

Astronomy and Astrophysics

Astronomy

9

Stars: Atmospheres, Sun, Techniques: Radial Velocities

Scientific paper

Convective motions in the solar photosphere produce line asymmetries that are traditionally studied using line bisectors observed with very high spectral resolution and signal-to-noise ratio. We study relative line-core shifts as a surrogate for bisectors, using the most current laboratory line positions of 298 Fe I lines in the Sun's visible flux spectrum and a new technique for determining line position. We show that this technique can be applied at significantly lower spectral resolutions and signal-to-noise ratios than has been done using bisectors. These line-core shifts show a clear dependence on both line strength and wavelength. The possibility of a dependence on the lower excitation energy is also examined.

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