Fig. 2
Model fits to lines of Si ii (right) and Si iii (left three panels) to the non-magnetic HgMn Star HD 78 316 (upper spectrum) and the magnetic Bp star BD-19 5044L (lower spectrum). The black lines are the observed spectra, red lines are the best fit model using the abundance derived from Si ii and the blue lines are the best fit model using the abundance derived from Si iii.
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