  Pre-supernova (SN) outbursts from massive stars may be driven by
hydrodynamical wave energy emerging from the core of the progenitor star during
late nuclear burning phases. Here, we examine the effects of wave heating in
stars containing little or no hydrogen, i.e., progenitors of type IIb/Ib SNe.
Because there is no massive hydrogen envelope, wave energy is thermalized near
the stellar surface where the overlying atmospheric mass is small but the
optical depth is large. Wave energy can thus unbind this material, driving an
optically thick, super-Eddington wind. Using 1D hydodynamic MESA simulations of
$\sim \! 5 \, M_\odot$ He stars, we find that wave heating can drive pre-SN
outbursts composed of a dense wind whose mass loss rate can exceed $\sim \! 0.1
\, M_\odot/{\rm yr}$. The wind terminal velocities are a few $100 \, {\rm
km}/{\rm s}$, and outburst luminosities can reach $\sim \! 10^6 \, L_\odot$.
Wave-driven outbursts may be linked with observed or inferred pre-SN outbursts
of type Ibn/transitional/transformational SNe, and pre-SN wave-driven mass loss
is a good candidate to produce these types of SNe. However, we also show that
non-linear wave breaking in the core of the star may prevent such outbursts in
stars with thick convective helium-burning shells. Hence, only a limited subset
of SN progenitors are likely to experience wave-driven pre-SN outbursts.
