Gravitational wave signals from 3D neutrino hydrodynamics simulations of core-collapse supernovae

By H. Andresen, B. Mueller, E. Mueller, H. J. M. Astrophysics, Garching, Physik Dept., Tum, Queen's University of Belfast, M. University. 2016

149 citations recorded by the source corpus.

We present gravitational wave (GW) signal predictions from four 3D multi-group neutrino hydrodynamics simulations of core-collapse supernovae of progenitors with 11.2 Msun, 20 Msun, and 27 Msun. GW emission in the pre-explosion phase strongly depends on whether the post-shock flow is dominated by the standing accretion shock instability (SASI) or convection and differs considerably from 2D models. SASI activity produces a strong signal component below 250 Hz through asymmetric mass motions in the gain layer and a non-resonant coupling to the proto-neutron star (PNS). Both convection- and SASI-dominated models show GW emission above 250 Hz, but with considerably lower amplitudes than in 2D. This is due to a different excitation mechanism for high-frequency l=2 motions in the PNS surface, which are predominantly excited by PNS convection in 3D. Resonant excitation of high-frequency surface g-modes in 3D by mass motions in the gain layer is suppressed compared to 2D because of smaller downflow velocities and a lack of high-frequency variability in the downflows. In the exploding 20 Msun model, shock revival results in enhanced low-frequency emission due to a change of the preferred scale of the convective eddies in the PNS convection zone. Estimates of the expected excess power in two frequency bands suggests that second-generation detectors will only be able to detect very nearby events, but that third-generation detectors could distinguish SASI- and convection-dominated models at distances of ~10 kpc.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/4250402f9b8f7cbfce790ae4bc6e100b00b67e6f

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Citations in the corpus

Characterizing the Gravitational Wave Signal from Core-collapse Supernovae (2018, methodology): “The combined observation of GWs, neutrinos, and photons (Nakamura et al. 2016) from the next Galactic CCSN could unveil the mechanism by which massive stars explode at the end of their lives, resolving a puzzle that has eluded the scientific community for more than 50 yr (Janka 2012; Burrows 2013; M”
Exploring Fundamentally Three-dimensional Phenomena in High-fidelity Simulations of Core-collapse Supernovae (2018, result): “This observation is in agreement with other analyses (Mueller & Janka 1997; Andresen et al. 2017) although other comparisons between the gravitational wave signature in 2D and 3D find much less of a suppression in 3D (Yakunin et al. 2017).”
Science case for the Einstein telescope (2019, background): “Besides, the Standing Accretion Shock Instability (SASI) [127, 128] which is an instability of the supernova shock wave itself is expected, in conjunction with turbulence, to modulate the accretion flow, to excite the proto-neutro star high frequency oscillation modes as well as to generate low freq”
The Gravitational Wave Signal from Core-collapse Supernovae (2018, methodology): “Aside from the possible SASI and neutrino signal, which are expected to operate at the frequencies .100 Hz (see Kuroda et al. 2016; Andresen et al. 2017), there is no other apparent mechanism that could fill this ‘excluded region’ of the spectrogram.”