Evolution of a supernova type Ia progenitor requires formation of a CO white dwarf , which implies a dependence on the C burning rate ( CBR ) .
It can also be affected by the recently identified possibility of C flame quenching by convective boundary mixing .
We present first results of our study of the combined effect of these two potential sources of uncertainty on the SN Ia progenitor evolution .
We consider the possibility that the CBR is higher than its currently recommended value by as much as a factor of 1000 if unidentified resonances are important , or that it is significantly lower because of the hindrance effect .
For stellar models that assume the Schwarzschild boundary for convection , the maximum initial mass for the formation of CO WDs increases from M _ { \mathrm { i } } \approx 5.5 M _ { \odot } for the CBR factor of 1000 to M _ { \mathrm { i } } \stackrel { > } { { } _ { \sim } } 7.0 M _ { \odot } for the CBR factor of 0.01 .
For C-flame quenching models , hybrid C-O-Ne WDs form for a range of initial mass of \Delta M _ { \mathrm { i } } \approx 1 M _ { \odot } , which increases a fraction of stars that form WDs capable of igniting C in a thermonuclear runaway .
The most extreme case is found for the CBR factor of 0.1 that is supported by the hindrance model .
This nuclear physics assumption , combined with C flame quenching , leads to the formation of a hybrid C-O-Ne WD with a mass of 1.3 M _ { \odot } .
Such WDs do not need to accrete much mass to reach the Chandrasekhar limit .