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We present theoretical models of type II supernova SN1993J. We show that a late-type progenitor can explain the initial sharp peak in the supernova light curve, provided that the progenitor had lost almost all of its hydrogen-rich envelope prior to the supernova event. Our hydrodynamical calculations suggest that the progenitor had an initial main-sequence mass of $\sim 15 M_{\odot}$, a residual hydrogen-rich envelope mass of $\sim 0.2 M_{\odot}$, and an explosion energy of $\sim 10^{51}$ ergs. In our model, the secondary brightening of the light curve is caused by the radioactive energy input from the decay of $\sim 0.1 M_{\odot}$ of ${\null}^{56}$Ni, and subsequently ${\null}^{56}$Co, produced in the explosion. The progenitor had most likely lost most of its hydrogen-rich envelope through mass transfer to a companion star, and we discuss the binary parameters which may lead to such a supernova event. From the binary parameters, we estimate the frequency of such events to be approximately $1$ in $20-30$ type II supernovae.
