Core-collapse supernovae

Core-collapse supernovae (CCSNe) have been known to explode, and recent theoretical success in reproducing these explosions permits the luxury of asking why. Their explosin mechanism - the turbulent neutrino-driven explosion of massive stars - presents an unsolved problem for over half a century, since the earliest simulations by Stirling Colgate in the 1960s. CCSNe are atomic factories, high-energy laboratories, galactic drivers, and compact remnant mills. Recent improvements in high-performance computing, stellar modeling, and neutrino physics have enabled a new generation of multi-dimensional simulations of core-collapse supernovae that produce robust explosions. I present the largest multidimensional suite of simulations to-date, from the first seconds of explosion in the core to weeks later until the shock reaches the stellar surface and slams into the circumstellar environment. I discuss the joint detectability of correlated neutrinos gravitational waves, and eventually light, from such events, which will illustrate the dynamics of the remnant neutron star, the explosion geometry, and global stellar instabilities. The results - ejecta kinematics, morphology, isotopic distribution, and signature templates - link observational and theoretical forays into core-collapse supernovae as Nature's astrophysical laboratories.