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We present a bolometric light curve model of Type IIn supernovae powered bysupernova ejecta colliding with a circumstellar medium. We estimate theconversion efficiency of the ejecta's kinetic energy to radiation at thereverse and forward shocks and find that a large density contrast makes adifference in the efficiency. The emission from the reverse shock can maintainhigh efficiency for a long time, and becomes important at the late phase of thelight curve. We first construct a semi-analytical model that is applicable tothe late phase of the light curve when the diffusion time of photons in theshocked region becomes negligible. We further develop radiation transfersimulations that incorporate these physical processes into the light curve. Thenumerical calculations predict light curves at early phases, which are testableby present and future short-cadence surveys. We compare our model with thebolometric light curve constructed from observations for a type IIn supernova2005ip. Due to the reduced efficiency at the forward shock, we find from ourmodel that the mass-loss rate of the progenitor star was $\approx 1\times10^{-2}\ {\rm M_\odot \ yr^{-1}}$ for a wind velocity of $100\ {\rm km \s^{-1}}$, an order of magnitude higher compared to previous work that usedsimple assumptions of the efficiency. This highlights the importance of takingthese two components into account when extracting the physical parameters fromobservations.

Type IIn Supernova Light Curves Powered by Forward and Reverse Shocks