deletions | additions       diff --git a/figures/emission_star3/caption.tex b/figures/emission_star3/caption.tex  index 09c2ca7..1a3dc09 100644  --- a/figures/emission_star3/caption.tex  +++ b/figures/emission_star3/caption.tex 
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\label{fig:emission1} \emph{Top of each panel:} observed FDBinary-extracted spectrum of Star 1 (red) together with a stellar template (dotted black line). \emph{Bottom of each panel:} difference between the observed and model spectra. Vertical lines show the position of each absorption line. Broadened Fe I magnetic-sensitive  lines indicates likely would indicate  Zeeman splitting \citep{har73}. Emission splitting, but this is not observed. Net emission  in the H$\alpha$ and Ca II {\rm Ca}\kern 0.1em{\sc ii}  lines is a  characteristic signature  of chromospheric magnetic activity. activity, but this is not observed either. Instead, the H$\alpha$ line is deeper and broader than the model.