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Massive stars undergo fundamental-mode and first-overtone radial pulsationswith periods of 100-1000 days as Red Supergiants (RSGs). At large amplitudes,these pulsations substantially modify the outer envelope's density structureencountered by the outgoing shock wave from the eventual core collapse of these$M>9M_\odot$ stars. Using Modules for Experiments in Stellar Astrophysics(MESA), we model the effects of fundamental-mode and first-overtone pulsationsin the RSG envelopes, and the resulting Type IIP supernovae (SNe) usingMESA+STELLA. We find that, in the case of fundamental mode pulsations, SNplateau observables such as the luminosity at day 50, $L_{50}$, time-integratedshock energy $ET$, and plateau duration $t_{\rm p}$ are consistent with radialscalings derived considering explosions of non-pulsating stars. Namely, most ofthe effect of the pulsation is consistent with the behavior expected for a starof a different size at the time of explosion. However, in the case of overtonepulsations, the Lagrangian displacement is not monotonic. Therefore, in suchcases, excessively bright or faint SN emission at different times reflects theunderdense or overdense structure of the emitting region near the SNphotosphere.

A Massive Star's Dying Breaths: Pulsating Red Supergiants and Their Resulting Type IIP Supernovae