Gravitational-wave signatures in successful vs. failed core-collapse supernovae

Kei Kotake

We will report the gravitational-wave (GW) radiation based on our 2D and 3D radiation-hydrodynamic simulations of core-collapse supernovae. In absence of rotation, we find that the gravitational waveform changes stochastically with time reflecting the chaotic growth of convection and fluid instability (so-called SASI) in the supernova cores. On the other hand, when the supernova cores rotate rapidly, we find that the stochasticity breaks down due to rotation, leading to a characteristic feature in the gravitational waveforms. To elucidate the GW radiation from *failed* core-collapse supernovae, we compute the GW waveforms in the context of collapsar scenario. Based on the 2D SRMHD collapsar simulations, we show that the GW signatures from collapsar could be viable up to 100 Mpc distance scales for the currently planned laser interferometers such as DECIGO. Since the event rates of gamma-ray bursts (GRBs) will be a few within a decade, we point out that the GW astronomy of GRBs can be feasible.