Core-collapse supernovae from massive stars are among the most energetic events in the universe. They liberate a mass-energy equivalent of ~15% of a solar mass in the collapse of their progenitor star's core. The majority (~99%) of this energy is carried away by neutrinos, while (~1%) is transferred to the kinetic energy of the explosive outflow. A smaller, yet still tremendous amount of energy is emitted in electromagnetic and gravitational waves.
The stellar collapse phenomenon and its range of outcomes pose a formidable theoretical and computational challenge. I discuss this challenge and review recent progress made in multi-dimensional simulations of the physical mechanism(s) believed responsible for converting the gravitational energy liberated in collapse into energy of the explosion. I outline how detections of gravitational waves and neutrinos from the next nearby core-collapse event can help to observationally probe dynamics and thermodynamics of the supernova engine.