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Supernovae (SNe) powered by interaction with circumstellar material provideevidence for intense stellar mass loss during the final years leading up tocore collapse. We have argued that during and after core neon burning, internalgravity waves excited by core convection can tap into the core fusion power andtransport a super-Eddington energy flux out to the stellar envelope,potentially unbinding up to ~ 1 solar mass of material. In this work, weexplore the internal conditions of SN progenitors using the MESA 1-D stellarevolution code, in search of those most susceptible to wave-driven mass loss.We focus on simple, order of magnitude considerations applicable to a widerange of progenitors. Wave-driven mass loss during core neon and oxygen fusionhappens preferentially in either lower mass (<~ 20 solar mass ZAMS) stars ormassive, sub-solar metallicity stars. Roughly 20 per cent of the SN progenitorswe survey can excite ~ 10^46 - 10^48 erg of energy in waves that canpotentially drive mass loss within a few months to a decade of core collapse.This energy can generate a circumstellar environment with 10^-3 - 1 solar massreaching ~ 100 AU before explosion. We predict a correlation between the energyassociated with pre-SN mass ejection and the time to core collapse, with themost intense mass loss preferentially happening closer to core collapse. Duringsilicon burning, a ~ 5 day long phase for our progenitor models, wave energymay inflate ~ 10^-3 - 1 solar mass of the stellar envelope to ~ 10 - 100s ofsolar radii. This suggests that some nominally compact SN progenitors (Type Ibcprogenitors) will have a significantly different SN shock breakout signaturethan traditionally assumed. We discuss the implications of our results for thecore-collapse SN mechanism, Type IIn SNe, Type IIb SNe from extendedprogenitors (e.g., SNe 1993j and 2011dh), and observed pre-SN outbursts.

Setting the Stage for Circumstellar Interaction in Core-Collapse Supernovae II: Wave-Driven Mass Loss in Supernova Progenitors