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The activity of massive stars approaching core-collapse can strongly affectthe appearance of the star and its subsequent supernova. Late-phase convectivenuclear burning generates waves that propagate toward the stellar surface,heating the envelope and potentially triggering mass loss. In this work, weimprove on previous one-dimensional models by performing two-dimensionalsimulations of the pre-supernova mass ejection phase due wave heat deposition.Beginning with stellar evolutionary models of a 15 $M_{\odot}$ red supergiantstar during core O-burning, we treat the energy deposition rate and duration asmodel parameters and examine the mass-loss dependence and the pre-explosionmorphology accordingly. Unlike one-dimensional models, density inversions dueto wave heating are smoothed by Rayleigh-Taylor instabilities, and the primaryeffect of wave heating is to radially expand the star's hydrogen envelope. Forlow heating rates with long durations, the expansion is nearly homologous,whereas high but short-lived heating can generate a shock that drives envelopeexpansion and results in a qualitatively different density profile at the timeof core-collapse. Asymmetries are fairly small, and large amounts of mass lossare unlikely unless the wave heating exceeds expectations. We discussimplications for pre-supernova stellar variability and supernovae light curves.

Hydrodynamic Simulations of Pre-Supernova Outbursts in Red Supergiants: Asphericity and Mass Loss