The Gravitational-Wave Signature of Core-Collapse Supernovae

The theory of core-collapse supernova (CCSN) explosions has been developed over the last six decades and is now a mature field at the interface of gravitational, particle, nuclear, statistical, and numerical physics. This theory is now buttressed by extensive numerical simulation and most 3D models now explode without artifice. The dominant gravitational-wave (GW) emission occurs during the post-shock turbulent phase in the neutrino-heated bubble bounded by the stalled (and early exploding) shock wave due to the associated violent non-radial inflow of mass plumes onto the inner proto-neutron star (PNS) core. By impinging upon the near-surface layers of the PNS, these plumes stochastically excite l=2 f-, p-, and g-modes. However, direct verification of explosion model details and the associated timelines are difficult to come by and gravitational wave signatures of this dynamical event would allow one to follow the theoretically expected sequence of events in real time. We will present in this talk state-of-the-art predictions of the signature of CCSNe as a function of progenitor mass and time. For the first time, our 3D models have captured the entire signal, not just the early phases. Features such as the excitation mechanisms, the oscillation modes, the bounce signatures, harmonic generation, and avoided crossings will be presented and discussed. Finally, we address the detectability of the emissions and features.