  Most massive stars experience binary interactions in their lifetimes that can
alter both the surface and core structure of the stripped star with significant
effects on their ultimate fate as core-collapse supernovae. However,
core-collapse supernovae simulations to date have focused almost exclusively on
the evolution of single stars. We present a systematic simulation study of
single and binary-stripped stars with the same initial mass as candidates for
core-collapse supernovae (11 - 21 M$_{\odot}$). Generally, we find that
binary-stripped stars core tend to be less compact, with a more prominent,
deeper silicon/oxygen interface, and explode preferentially to the
corresponding single stars of the same initial mass. Such a dichotomy of
behavior between these two modes of evolution would have important implications
for supernovae statistics, including the final neutron star masses, explosion
energies, and nucleosynthetic yields. Binary-stripped remnants are also well
poised to populate the possible mass gap between the heaviest neutron stars and
the lightest black holes. Our work presents an improvement along two fronts, as
we self-consistently account for the pre-collapse stellar evolution and the
subsequent explosion outcome. Even so, our results emphasize the need for more
detailed stellar evolutionary models to capture the sensitive nature of
explosion outcome.
