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We examine how tides, stellar evolution, and magnetic braking shape therotation period (P$_{rot}$) evolution of low-mass stellar binaries up toorbital periods (P$_{orb}$) of 100 d across a wide range tidal dissipationparameters using two common equilibrium tidal models. We find that manybinaries with P$_{orb} < 20$ d tidally lock, and most with $P_{orb} < 4$ dtidally lock into synchronous rotation on circularized orbits. At shortP$_{orb}$, tidal torques produce a population of fast rotators that single-staronly models of magnetic braking fail to produce. In many cases, we show thatthe competition between magnetic braking and tides produces a population ofsubsynchronous rotators that persists for Gyrs, even in short P$_{orb}$binaries, qualitatively reproducing the subsynchronous eclipsing binaries (EBs)discovered in the Kepler field by Lurie et al. (2017). Both equilibrium tidalmodels predict that binaries can tidally-interact out to P$_{orb} \approx 80$d, while the Constant Phase Lag tidal model predicts that binaries can tidallylock out to P$_{orb} \approx 100$ d. Tidal torques often force the P$_{rot}$evolution of stellar binaries to depart from the long-term magneticbraking-driven spin down experienced by single stars, revealing that P$_{rot}$is not be a valid proxy for age in all cases, i.e. gyrochronology canunderpredict ages by up to $300\%$ unless one accounts for binarity. We suggestthat accurate determinations of orbital eccentricties and P$_{rot}$ can be usedto discriminate between which equilibrium tidal models best describes tidalinteractions in low-mass binary stars.

Rotation Period Evolution in Low-Mass Binary Stars: The Impact of Tidal Torques and Magnetic Braking