  Considering the uncertainties of the C-burning rate (CBR) and the treatment
of convective boundaries, Chen et al. (2014) found that there is a regime where
it is possible to form hybrid CONe white dwarfs (WDs), i.e. ONe WDs with
carbon-rich cores. As these hybrid WDs can be as massive as 1.30 $M_{\odot}$,
not much mass needs to be accreted for these objects to reach the Chandrasekhar
limit and to explode as Type Ia supernovae (SNe Ia). We have investigated their
contribution to the overall SN Ia birth rate and found that such SNe Ia tend to
be relatively young with typical time delays between 0.1 and 1 Gyr, where some
may be as young as 30 Myr. SNe Ia from hybrid CONe WDs may contribute several
percent to all SNe Ia, depending on the common-envelope ejection efficiency and
the CBR. We suggest that these SNe Ia may produce part of the 2002cx-like SN Ia
class.
