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Interactions between convective shells in evolved massive stars have beenlinked to supernova impostors, to the production of the odd-Z elements Cl, K,and Sc, and they might also help generate the large-scale asphericities thatare known to facilitate shock revival in supernova explosion models. Weinvestigate the process of ingestion of C-shell material into a convectiveO-burning shell, including the hydrodynamic feedback from the nuclear burningof the ingested material. Our 3D hydrodynamic simulations span almost 3 dex inthe total luminosity $L_\mathrm{tot}$. All but one of the simulations reach aquasi-stationary state with the entrainment rate and convective velocityproportional to $L_\mathrm{tot}$ and $L_\mathrm{tot}^{1/3}$, respectively.Carbon burning provides $14\,$--$\,33\%$ of the total luminosity, depending onthe set of reactions considered. Equivalent simulations done on $768^3$ and$1152^3$ grids are in excellent quantitative agreement. The flow is dominatedby a few large-scale convective cells. An instability leading to large-scaleoscillations with Mach numbers in excess of $0.2$ develops in an experimentalrun with the energy yield from C burning increased by a factor of 10. This runrepresents most closely the conditions expected in a violent O-C shell merger,which is a potential production site for odd-Z elements such as K and Sc andwhich may seed asymmetries in the supernova progenitor. 1D simulations mayunderestimate the energy generation from the burning of ingested material by asmuch as a factor two owing to their missing the effect of clumpiness ofentrained material on the nuclear reaction rate.

3D hydrodynamic simulations of C ingestion into a convective O shell