Observing Convection: FeI Lineshifts in the Central Intensity Spectrum of the Sun

Astronomy and Astrophysics – Astronomy

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Scientific paper

The central intensity spectrum of the Sun has been used to determine the convective line core shifts for 1112 FeI lines. The distributions of the line core shifts with respect to wavelength, excitation energy and line depth provide insight into the convective velocities within the solar photosphere. The FeI distributions in the visible have been compared with previous work on the Solar Flux spectrum to investigate the effects of limb darkening . The impact of variations in continuous opacity on the shapes of these distributions is also discussed. When the line core shift distributions are examined clear evidence of a dependence on line strength is found at all wavelengths, and sensitivities to wavelength are found at shorter wavelengths for FeI. Atmospheric modeling has been done to determine the corresponding physical depths of formation for a variety of simulated lines at different wavelengths and strengths. The combination of the line core shift distributions with these models allow for an approximate reconstruction of the velocity structure for the Solar photosphere and a more thorough examination of the noted dependencies.

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