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Eruptive mass loss likely produces the energetic outbursts observed from somemassive stars before they undergo core-collapse supernovae (CCSNe). Theresulting dense circumstellar medium (CSM) may also cause the subsequent SNe tobe observed as Type IIn events. The leading hypothesis of the cause of theseoutbursts is the response of the envelope of the red supergiant (RSG)progenitor to energy deposition in the months to years prior to collapse. Earlytheoretical studies of this phenomena were limited to 1D, leaving the 3Dconvective RSG structure unaddressed. Using FLASH's hydrodynamic capabilities,we explore the 3D outcomes by constructing convective RSG envelope models anddepositing energies less than the envelope binding energies on timescalesshorter than the envelope dynamical time deep within them. We confirm the 1Dprediction of an outward moving acoustic pulse steepening into a shock,unbinding the outermost parts of the envelope. However, we find that theinitial 2-4 km/s convective motions seed the intrinsic convective instabilityassociated with the high entropy material deep in the envelope, enabling gasfrom deep within the envelope to escape, increasing the amount of ejected masscompared to an initially "quiescent" envelope. The 3D models reveal a richdensity structure, with column densities varying by 10x along different linesof sight. Our work highlights that the 3D convective nature of RSG envelopesimpacts our ability to reliably predict the outburst dynamics, the amount, andthe spatial distribution of the ejected mass associated with deep energydeposition.

3D Hydrodynamics of Pre-supernova Outbursts in Convective Red Supergiant Envelopes