  Recent studies have shown that for suitable initial conditions both super-
and sub-Chandrasekhar mass carbon-oxygen white dwarf mergers produce explosions
similar to observed SNe Ia. The question remains, however, how much fine tuning
is necessary to produce these conditions. We performed a large set of SPH
merger simulations, sweeping the possible parameter space. We find trends for
merger remnant properties, and discuss how our results affect the viability of
our recently proposed sub-Chandrasekhar merger channel for SNe Ia.
