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We identify a sample of near-equal mass wide binary M dwarf systems from theSLoWPoKES catalog of common proper-motion binaries and obtain follow-upobservations of their chromospheric activity as measured by the H$\alpha$emission line. We present optical spectra for both components of 48 candidate Mdwarf binaries, confirming their mid-M spectral types. Of those 48 coevalpairs, we find eight with H$\alpha$ emission from both components, three withweak emission in one component and no emission in the other, and 37 with twoinactive components. We find that of the eleven pairs with at least one activecomponent, only three follow the net trend of decreasing activity strength$L_{\rm H\alpha}/L_{\rm bol}$ with later spectral type. The difference inquiescent activity strength between the A and B components is larger than whatwould be expected based on the small differences in color (mass). For fivebinaries with two active components, we present 47 hours of time-resolvedspectroscopy, observed on the ARC 3.5-m over twelve different nights. For fourof the five pairs, the slightly redder (B) component exhibits a higher level ofH$\alpha$ emission during the majority of the observations and the redderobjects are the only components to flare. The full range of H$\alpha$ emissionobserved on these variable mid-M dwarfs is comparable to the scatter inH$\alpha$ emission found in single-epoch surveys of mid-M dwarfs, indicatingthat variability could be a major factor in the spread of observed activitystrengths. We also find that variability is independent of both activitystrength and spectral type.

H$\alpha$ Emission From Active Equal-mass, Wide M Dwarf Binaries