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We present the first three-dimensional, full-star simulations of convectionin a white dwarf preceding a Type Ia supernova, specifically the last few hoursbefore ignition. For these long-time calculations we use our low Mach numberhydrodynamics code, MAESTRO, which we have further developed to treat sphericalstars centered in a three-dimensional Cartesian geometry. The main changerequired is a procedure to map the one-dimensional radial base state to andfrom the Cartesian grid. Our models recover the dipole structure of the flowseen in previous calculations, but our long-time integration shows that theorientation of the dipole changes with time. Furthermore, we show thedevelopment of gravity waves in the outer, stable portion of the star. Finally,we evolve several calculations to the point of ignition and discuss the rangeof ignition radii.

Low Mach Number Modeling of Type Ia Supernovae. IV. White Dwarf Convection