Fig. 9.
Example fit of the different inversions (row (e), x = 7.9). We only fitted Stokes Q, U, and V in the λ8542, λ6301, and 6302 lines. The fits for the Ca II H, Fe Iλ6301, and Mg II h lines are not shown because they are virtually identical to those in their partnering lines. At the considered noise level, all Q and U signals are below the noise level in all chromospheric lines.
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