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A number of astrophyical transients originating from stellar explosions arepowered by the collision of the ejected material with the circumstellar medium,which efficiently produces thermal radiation via shock dissipation. Weinvestigate how such interaction-powered transients are distributed in the peakbolometric luminosity vs the rise time phase space. Taking the advantage ofless time-consuming one-dimensional simulations with spherical symmetry, wecalculated more than 500 models with different circumstellar mass and radius,ejecta mass and energy, and chemical compositions. The peak bolometricluminosity, the total radiated energy, and the rise time of theinteraction-powered emission are measured for each simulated light curve. Weconsider how these characteristic quantities are determined as a function ofthe model parameters and discuss possible implications for the observedpopulations of (potential) interaction-powered transients, such as type IInsupernovae and fast blue optical transients.

A systematic study on the rise time-peak luminosity relation for bright optical transients powered by wind shock breakout