A general property of galaxy disks is that the stellar component should have a rotational velocity that lags behind that of the gas components, a property known as asymmetric drift. The physical mechanism behind this is that gas efficiently dissipates energy allowing it to settle into orbits dictated by the circular speed of the galactic potential, whereas stars are collisionless and retain any non-circular motions that they have accrued over their dynamical history. Because of their detailed relation to the galactic potential and the stellar phase-space distribution function, measurements of asymmetric drift are a fundamental dynamical property of disk galaxies; however, they represent relatively undiscovered territory given the paucity of such measurements in the literature. I will discuss preliminary phenomenological assessments of asymmetric drift seen in the disk-galaxy population observed by MaNGA to-date. I will also discuss the use of these measurements in calculating disk-only masses (as opposed to total enclosed masses), as well as prospects for assessing the dynamical heating rate in external galaxies, which may be the cause of the observed color–velocity-dispersion relation seen in the solar neighborhood of the Milky Way.