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We explore the effects of the residual $\mathrm{^{12}C}$ present inoxygen-neon white dwarfs (ONe WDs) on their evolution towards accretion-inducedcollapse (AIC). We produce a set of ONe WD models using MESA and illustrate howthe amount and location of the residual carbon depends on the initial mass ofthe star and assumptions about rotation and convective overshooting. We find awide range of possible $\mathrm{^{12}C}$ mass fractions roughly ranging from0.1 to 10 per cent. Convection and thermohaline mixing that occurs as the ONeWDs cool leads to nearly homogeneous interior compositions by the time that AICwould occur. We evolve these ONe WD models and some toy WD models towards AICand find that regardless of the carbon fraction, the occurrence of Urca-processcooling due to $\mathrm{^{23}Na}$ implies that the models are unlikely to reachcarbon ignition before electron captures on $\mathrm{^{24}Mg}$ occur.Difficulties associated with modeling electron-capture-driven convectiveregions in these ONe WDs prevent us from evolving our MESA models all the wayto thermonuclear oxygen ignition and the onset of collapse. Thus, firmconclusions about the effect of carbon on the final fates of these objectsawait improved modeling. However, it is clear that the inclusion of residualcarbon can shift the evolution from that previously described in the literatureand should be included in future models.

Residual Carbon in Oxygen-Neon White Dwarfs and its Implications for Accretion-Induced Collapse