Gravitational Wave Emission from Long-Term Self-Consistent Two-dimensional Core-Collapse Supernova Models

Abstract

We report gravitational-wave (GW) signatures based on two-dimensional (2D) neutrino-radiation hydrodynamics simulations of core-collapse supernovae (CCSNe). Using multiple progenitor models, we present systematic analysis of the GW emission from the self-consistent 2D models. We find that the total GW energies emitted during the simulation become higher for models with progenitors' high compactness. This is because the high compactness leads to more energetic explosions, where non-spherical hydrodynamic motions associated with neutrino-driven convection and the StandingAccretion-Shock-Instability develop much more violently. On the other hand, we show that the GW energies become smaller for high-compactness models that fail to explode by the neutrino-driven mechanism. This is because non-spherical motions in the postbounce core get gradually weaker with the decreasing mass accretion rate to the proto-neutron star, which leads to the smaller GW amplitudes in the long postbounce evolution. We discuss the detectability of the GW signals from both the successful and unsuccessful models using the advanced GW detectors including LIGO and KAGRA.