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Pre-supernova (SN) outbursts from massive stars may be driven byhydrodynamical wave energy emerging from the core of the progenitor star duringlate nuclear burning phases. Here, we examine the effects of wave heating instars containing little or no hydrogen, i.e., progenitors of type IIb/Ib SNe.Because there is no massive hydrogen envelope, wave energy is thermalized nearthe stellar surface where the overlying atmospheric mass is small but theoptical depth is large. Wave energy can thus unbind this material, driving anoptically thick, super-Eddington wind. Using 1D hydodynamic MESA simulations of$\sim \! 5 \, M_\odot$ He stars, we find that wave heating can drive pre-SNoutbursts 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 $100 \, {\rmkm}/{\rm s}$, and outburst luminosities can reach $\sim \! 10^6 \, L_\odot$.Wave-driven outbursts may be linked with observed or inferred pre-SN outburstsof type Ibn/transitional/transformational SNe, and pre-SN wave-driven mass lossis a good candidate to produce these types of SNe. However, we also show thatnon-linear wave breaking in the core of the star may prevent such outbursts instars with thick convective helium-burning shells. Hence, only a limited subsetof SN progenitors are likely to experience wave-driven pre-SN outbursts.

Pre-Supernova Outbursts via Wave Heating in Massive Stars II: Hydrogen-poor Stars