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A proposed setting for thermonuclear (Type Ia) supernovae is a white dwarfthat has gained mass from a companion to the point of carbon ignition in thecore. There is a simmering phase in the early stages of burning that involvesthe formation and growth of a core convection zone. One aspect of this phase isthe convective Urca process, a linking of weak nuclear reactions to convectionthat may alter the composition and structure of the white dwarf. ConvectiveUrca is not well understood and requires 3D fluid simulations to realisticallymodel. Additionally, the convection is relatively slow (Mach number less than0.005) so a low-Mach method is needed to make simulating computationallyfeasible. Using the MAESTROeX low-Mach hydrodynamics code, we investigaterecent changes to how the weak reactions are modeled in the convective Urcasimulations. We present results that quantify the changes to the reaction ratesand their impact on the evolution of the simulation.

Sensitivity of 3D Convective Urca Simulations to Changes in Urca Reactions