Abstract
A comparison is made of synthetic and empirical analyses for the 4571 Å line of Mg i. First, several different inversion techniques are applied to synthetic line profiles. The results show that at least some of these techniques are able to correctly reproduce the input atmosphere to a reasonable degree. Secondly, these same techniques are applied to equivalent observational data. In this case some of the techniques yield results that can be shown to be of comparable quality to the synthetic analysis. I conclude that although the synthetic method is the best method to use in analyzing observations, some of the simpler empirical methods produce acceptable results in specified restricted cases.
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Altrock, R.C. The formation of Mg i 4571 Å in the solar atmosphere. Sol Phys 34, 37–56 (1974). https://doi.org/10.1007/BF00149598
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DOI: https://doi.org/10.1007/BF00149598