Gravitational waves from 3D MHD core collapse simulations

TL;DR

This paper analyzes gravitational wave signals from 3D magnetohydrodynamic simulations of core-collapse supernovae, revealing different emission mechanisms and assessing detectability by LIGO detectors.

Contribution

First 3D MHD simulations of core-collapse supernovae analyzing gravitational waves with detailed physics and nonaxisymmetric effects.

Findings

Type I gravitational wave signals at bounce

Nonaxisymmetric emission from dynamical instability in one model

Detectability of signals by LIGO and Advanced LIGO

Abstract

We present the gravitational wave analysis from rotating (model s15g) and nearly non-rotating (model s15h) 3D MHD core collapse supernova simulations at bounce and the first couple of ten milliseconds afterwards. The simulations are launched from 15M_{\odot} progenitor models stemming from stellar evolution calculations. Gravity is implemented by a spherically symmetric effective general relativistic potential. The input physics uses the Lattimer-Swesty equation of state for hot, dense matter and a neutrino parametrisation scheme that is accurate until the first few ms after bounce. The 3D simulations allow us to study features already known from 2D simulations as well as nonaxisymmetric effects. In agreement with recent results we find only type I gravitational wave signals at core bounce. In the later stage of the simulations, one of our models (s15g) shows nonaxisymmetric gravitational wave emission caused by a low T/|W| dynamical instability, while the other model radiates gravitational waves due to a convective instability in the protoneutron star. The total energy released in gravitational waves within the considered time intervals is 1.52\times10^{-7}M_{\odot} (s15g) and 4.72\times10^{-10}M_{\odot} (s15h). Both core collapse simulations indicate that corresponding events in our Galaxy would be detectable either by the LIGO or Advanced LIGO detector.