core via the excitation of non-radial pulsations [@couch:15b]. These create perturbations from which convection will grow after core bounce.

Given the above, multi-D simulations are essential for studying the dynamics of the supernova engine.

The rapid increase of compute power since the early 1990s has facilitated increasingly detailed 2D radiation-hydrodynamics simulations over the past two and a half decades. 3D simulations with simplified neutrino treatments have been carried out since the early 2000s. The first 3D neutrino radiation-hydrodynamics simulations have become possible only in the past few years, thanks to the compute power of large petascale systems like US NSF/NCSA Blue Waters, US DOE/ORNL Titan or the Japanese K computer.

Core-Collapse Supernova Simulation Codes
========================================

Many 1D codes exist, some are no longer in use, and one is open source and free to download (<http://GR1Dcode.org>). There are $\sim$$10$ (depending on how one counts) multi-D core-collapse supernova simulation codes in the community. Many, in particular the 3D codes, follow the design encapsulated by Figure \[fig:components\]. They employ a simulation framework (e.g., `FLASH`, <http://flash.uchicago.edu/site/flashcode/> or `Cactus` <http://cactuscode.org>) that handles domain decomposition, message passing, memory management, AMR, coupling of different physics components, execution scheduling, and I/O.

Given the tremendous memory requirement and FLOP-consumption 