Cluster Disruption: Combining Theory and Observations

We review the theory and observations of star cluster disruption. The three main phases and corresponding typical timescales of cluster disruption are: I) Infant Mortality (∼10⁷ yr), II) Stellar Evolution (∼10⁸ yr) and III) Tidal relaxation (∼10⁹ yr). During all three phases there are additional tidal external perturbations from the host galaxy. In this review we focus on the physics and observations of Phase I and on population studies of Phases II & III and external perturbations (concentrating on cluster-GMC interactions). Particular attention is given to the successes and short-comings of the Lamers cluster disruption law, which has recently been shown to stand on a firm physical footing.