All stars rotate, with periods ranging from milliseconds (for some neutron stars) to years (for some supergiants). Cool main-sequence stars with surface convection zones (Sun-like stars) show less range, but still span periods from fractions of a day to months. Our current understanding says that young stars rotate rapidly, but are eventually spun down by the torque from a magnetized stellar wind. To explain the details of rotational period distributions in not-too-old star clusters, the theory invokes other processes, notably a moderately long-lived (few hundred MY) decoupling of the rotation of the stellar convection zone from that of the interior. In this talk, I will first review the observational and theoretical arguments that lead to this picture. Then I will describe a modest variant to an alternative explanation for the observations that was first suggested by Sydney Barnes. It retains the notion of magnetized wind braking but does not require young-star convection zones to rotate independently of their radiative interiors. A desirable feature of this view is that if it is shown to be correct, we may as a result learn something fundamental about stellar dynamos. Last, I will discuss how one might choose between these two pictures. Unsurprisingly, time-domain observations are the key; LCOGT's world-wide network of robotic telescopes is ideally suited to provide much of the necessary data.