  Motivated by their role as the direct or indirect source of many of the
elements in the Universe, numerical modeling of core collapse supernovae began
more than five decades ago. Progress toward ascertaining the explosion
mechanism(s) has been realized through increasingly sophisticated models, as
physics and dimensionality have been added, as physics and numerical modeling
have improved, and as the leading computational resources available to modelers
have become far more capable. The past five to ten years have witnessed the
emergence of a consensus across the core collapse supernova modeling community
that had not existed in the four decades prior. For the majority of progenitors
- i.e., slowly rotating progenitors - the efficacy of the delayed shock
mechanism, where the stalled supernova shock wave is revived by neutrino
heating by neutrinos emanating from the proto-neutron star, has been
demonstrated by all core collapse supernova modeling groups, across progenitor
mass and metallicity. With this momentum, and now with a far deeper
understanding of the dynamics of these events, the path forward is clear. While
much progress has been made, much work remains to be done, but at this time we
have every reason to be optimistic we are on track to answer one of the most
important outstanding questions in astrophysics: How do massive stars end their
lives?
