Binary Chandrasekhar-mass white dwarfs accreting mass from non-degenerate stellar companions through the single-degenerate channel have reigned for decades as the leading explanation of Type Ia supernovae. Yet, a coherent theoretical explanation has not yet emerged to explain the expected properties of the canonical near-Chandrasekhar-mass white dwarf model. Such near-Chandrasekhar-mass SNe Ia are preceded by a simmering phase within the convective core of the white dwarf, leading to the ignition of one or more flame bubbles scattered across the core.