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Fully convective M dwarfs typically remain rapidly rotating and magneticallyactive for billions of years, followed by an abrupt and mass-dependenttransition to slow rotation and quiescence. A robust understanding of thisprocess is complicated by difficulties in estimating M-dwarf ages and potentialdependencies on other variables such as birth environment or metallicity. Toisolate the effect of mass, we consider M dwarfs in wide binaries. We identify67 widely separated, fully convective (0.08-0.35M$_\odot$) M-dwarf binarysystems using Gaia and measure the H$\alpha$ feature for each component. Weclassify the pairs into three categories: systems where both components areactive, systems where both are inactive, and candidate transition systems,where one component is active and the other inactive. We gatherhigher-resolution spectra of the candidate transition systems to verify thattheir behavior does not result from an unresolved third component, yielding onenew triple with surprising activity levels. Neglecting this triple, we find 22active, 36 inactive, and 8 transition pairs. Our results are consistent withthe epoch of spindown for these binaries being primarily determined by mass,with mild second-order effects; we place a 1$\sigma$ upper limit of 0.5Gyr or25% on the dispersion in the mass-dependent spindown relation. Our findingssuggest that the large dispersion in spindown epoch previously observed forfield stars of a given mass may stem from differences in birth environment, inaddition to modest intrinsic stochasticity. We also see evidence that the widebinary population is dispersed over time due to dynamical processing.

The Mass Dependence of H{\alpha} Emission and Stellar Spindown for Fully Convective M Dwarfs