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Title:
Solar granulation - Influence of convection on spectral line asymmetries and wavelength shifts
Authors:
Dravins, D.; Lindegren, L.; Nordlund, A.
Affiliation:
AA(Royal University Observatory, Lund, Sweden), AB(Royal University Observatory, Lund, Sweden), AC(Nordisk Institut for Teoretisk Atomfysik, Copenhagen, Denmark)
Publication:
Astronomy and Astrophysics, vol. 96, no. 1-2, Mar. 1981, p. 345-364. Research supported by the Statens Naturvetenskapliga Forskningsrad, Statens Naturvidenskabelige Forskningsrad, and Danish Space Board. (A&A Homepage)
Publication Date:
03/1981
Category:
Solar Physics
Origin:
STI
NASA/STI Keywords:
Convective Flow, Frequency Shift, Line Shape, Photosphere, Solar Granulation, Solar Spectra, Abundance, Asymmetry, Iron, Light Scattering, Solar Atmosphere, Spectral Line Width, Sunlight
Bibliographic Code:
1981A&A....96..345D

Abstract

The observed shapes and shifts of 311 Fe I lines in the spectrum of solar disk center and also of integrated sunlight are investigated. Line shapes are described using bisectors, and the dependence of these on line strength, excitation potential, and wavelength region is analyzed. A theoretical model atmosphere incorporating radiation-coupled, time-dependent hydrodymamics of solar convection is used to compute synthetic photospheric spectral lines. These lines exhibit asymmetries and wavelength shifts, and the observed bisector behavior can be closely reproduced. The detailed properties of, for example, convective motions and changing granulation constrast with wavelength manifest themselves in the detailed bisector shapes. It is confirmed that convection is the principal cause of solar line shifts, and errors in other suggested explanations are pointed out. It is concluded that the study of line shapes and shifts is a powerful tool for the analysis of solar photospheric convection.

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Physics
arXiv e-prints