\label{fig:emission1}Top of each panel: observed FDBinary-extracted spectrum of Star 1 (red) together with a stellar template (dotted black line). Bottom of each panel: difference between the observed and model spectra. Vertical lines show the position of each absorption line. Broadened magnetic-sensitive lines would indicate Zeeman splitting, but this is not observed. Net emission in the \(\rm{H}\alpha\) and Caii lines is a characteristic signature of chromospheric magnetic activity, but this is not observed either. Instead, the \(\rm{H}\alpha\) line is deeper and broader than the model.