Ba II 4554A Resonance Line Formation in the Solar Atmosphere

Details Ba II 4554A Resonance Line Formation in the Solar Atmosphere Ba II 4554A Resonance Line Formation in the Solar Atmosphere

Apr 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005ysc..conf...71o&link_type=abstract

12th Young Scientists' Conference on Astronomy and Space Physics, held in Kyiv, Ukraine, April 19-23, 2005, Eds.: Simon, A.; Gol

Physics

Space Physics

Scientific paper

We investigate non-LTE radiative transfer in the the Ba II 4554 A line in the Solar atmosphere. This line is particularly suited to measure non thermal motions in the solar photosphere. It is also used in Stokes vector spectropolarimetry. NLTE spectral formation modeling is a necessary step in the formulation of reliable quantitative data interpretation through numerical inversion. The first phase of the work includes creation of a reliable model of the Ba II atom. It includes: energy levels, oscillator strengths for the selected bb-transitions and bf-transitions probabilities. We also take into account the hyper fine structure and isotopic splitting. Next step is to calculate departure coefficients for Ba II through numerical solution of the radiative transfer equations. When these coefficients are derived it is possible to apply inversion techniques to spectral observations in this line.

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