Left: Time evolution of H I, He I, He II photon luminosities Q(t), number of photons emitted per unit time, for the three wind prescriptions: optically thick and homogeneous winds, partially clumpy, and highly clumped close to optically thin winds. The results shown are for non-rotating solar metallicity stars and for a star-cluster mass of 10⁶ M_⊙. Right: Cumulative photon emission, N_γ = ∫₀^TQ(t) dt, as a function of time T for the same parameters.