The dependence of the evolution of Type Ia SN progenitors on the C-burning rate uncertainty and parameters of convective boundary mixing

Abstract

Figure 1: The highest masses of the CO cores and the lowest masses of the ONe cores (top), and the initial masses of the stars that produce the highest CO core masses and the lowest ONe core masses (bottom), all plotted against the carbon burning rate (CBR) factor. These models include convective boundary mixing for C burning. The mass range between CO and ONe WDs is occupied by C-O-Ne hybrid core models.