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We present a study of the statistical flare rates of M dwarfs (dMs) withclose white dwarf (WD) companions (WD+dM; typical separations < 1 au). Ourprevious analysis demonstrated that dMs with close WD companions are moremagnetically active than their field counterparts. One likely implication ofhaving a close binary companion is increased stellar rotation throughdisk-disruption, tidal effects, and/or angular momentum exchange; increasedstellar rotation has long been associated with an increase in stellar activity.Previous studies show a strong correlation between dMs that are magneticallyactive (showing H{\alpha} in emission) and the frequency of stellar flarerates. We examine the difference between the flare rates observed in closeWD+dM binary systems and field dMs. Our sample consists of a subset of 181close WD+dM pairs from Morgan et al. (2012) observed in the Sloan Digital SkySurvey Stripe 82, where we obtain multi-epoch observations in the Sloanugriz-bands. We find an increase in the overall flaring fraction in the closeWD+dM pairs (0.09$\pm$0.03%) compared to the field dMs (0.0108$\pm$0.0007%;Kowalski et al. 2009) and a lower flaring fraction for active WD+dMs(0.05$\pm$0.03%) compared to active dMs (0.28$\pm$0.05%; Kowalski et al. 2009).We discuss how our results constrain both the single and binary dM flare rates.Our results also constrain dM multiplicity, our knowledge of the Galactictransient background, and may be important for the habitability of attendingplanets around dMs with close companions.

Using Close White Dwarf + M Dwarf Stellar Pairs to Constrain the Flare Rates in Close Stellar Binaries