  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 (~10^7 yr), II) Stellar Evolution (~10^8 yr) and III) Tidal
relaxation (~10^9 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.
