  Supernovae (SNe) powered by interaction with circumstellar material provide
evidence for intense stellar mass loss during the final years leading up to
core collapse. We have argued that during and after core neon burning, internal
gravity waves excited by core convection can tap into the core fusion power and
transport a super-Eddington energy flux out to the stellar envelope,
potentially unbinding up to ~ 1 solar mass of material. In this work, we
explore the internal conditions of SN progenitors using the MESA 1-D stellar
evolution code, in search of those most susceptible to wave-driven mass loss.
We focus on simple, order of magnitude considerations applicable to a wide
range of progenitors. Wave-driven mass loss during core neon and oxygen fusion
happens preferentially in either lower mass (<~ 20 solar mass ZAMS) stars or
massive, sub-solar metallicity stars. Roughly 20 per cent of the SN progenitors
we survey can excite ~ 10^46 - 10^48 erg of energy in waves that can
potentially 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 mass
reaching ~ 100 AU before explosion. We predict a correlation between the energy
associated with pre-SN mass ejection and the time to core collapse, with the
most intense mass loss preferentially happening closer to core collapse. During
silicon burning, a ~ 5 day long phase for our progenitor models, wave energy
may inflate ~ 10^-3 - 1 solar mass of the stellar envelope to ~ 10 - 100s of
solar radii. This suggests that some nominally compact SN progenitors (Type Ibc
progenitors) will have a significantly different SN shock breakout signature
than traditionally assumed. We discuss the implications of our results for the
core-collapse SN mechanism, Type IIn SNe, Type IIb SNe from extended
progenitors (e.g., SNe 1993j and 2011dh), and observed pre-SN outbursts.
