GENERAL-RELATIVISTIC SIMULATIONS OF THREE-DIMENSIONAL CORE-COLLAPSE SUPERNOVAE

By Christian D. Ott, E. Abdikamalov, P. Mösta, Roland Haas, S. Drasco, E. O’Connor, Christian Reisswig, C. Meakin, Erik Schnetter. 2012

140 citations recorded by the source corpus.

We study the three-dimensional (3D) hydrodynamics of the post-core-bounce phase of the collapse of a 27 M☉ star and pay special attention to the development of the standing accretion shock instability (SASI) and neutrino-driven convection. To this end, we perform 3D general-relativistic simulations with a three-species neutrino leakage scheme. The leakage scheme captures the essential aspects of neutrino cooling, heating, and lepton number exchange as predicted by radiation-hydrodynamics simulations. The 27 M☉ progenitor was studied in 2D by Müller et al., who observed strong growth of the SASI while neutrino-driven convection was suppressed. In our 3D simulations, neutrino-driven convection grows from numerical perturbations imposed by our Cartesian grid. It becomes the dominant instability and leads to large-scale non-oscillatory deformations of the shock front. These will result in strongly aspherical explosions without the need for large-scale SASI shock oscillations. Low-ℓ-mode SASI oscillations are present in our models, but saturate at small amplitudes that decrease with increasing neutrino heating and vigor of convection. Our results, in agreement with simpler 3D Newtonian simulations, suggest that once neutrino-driven convection is started, it is likely to become the dominant instability in 3D. Whether it is the primary instability after bounce will ultimately depend on the physical seed perturbations present in the cores of massive stars. The gravitational wave signal, which we extract and analyze for the first time from 3D general-relativistic models, will serve as an observational probe of the postbounce dynamics and, in combination with neutrinos, may allow us to determine the primary hydrodynamic instability.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/03b3a1f3224a81c23350d26fa9337d67a24126e5

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Citations in the corpus

THE ROLE OF TURBULENCE IN NEUTRINO-DRIVEN CORE-COLLAPSE SUPERNOVA EXPLOSIONS (2014, methodology): “We include the effects of heating, cooling, and electron fraction evolution due to neutrinos via an approximate, rayby-ray, multi-species leakage scheme (O’Connor & Ott 2010; Ott et al. 2013).”
Three-dimensional GRMHD Simulations of Neutrino-cooled Accretion Disks from Neutron Star Mergers (2017, methodology): “Such leakage schemes are widely used in both core-collapse supernova and compact-binary merger simulations (e.g., van Riper & Lattimer 1981; Ruffert et al. 1996; Rosswog & Liebendörfer 2003; Sekiguchi et al. 2011; Ott et al. 2013; Radice et al. 2016; Perego et al. 2016).”
A COMPARISON OF TWO- AND THREE-DIMENSIONAL NEUTRINO-HYDRODYNAMICS SIMULATIONS OF CORE-COLLAPSE SUPERNOVAE (2013, background): “…multi-D hydrodynamic feedback of neutrino-driven convection and 1 Note that general relativity (GR, e.g., Müller et al. (2012); Kuroda et al. (2012); Ott et al. (2013)) and detailed weak interactions (e.g., Langanke et al. (2008); Furusawa et al. (2013)) are considered as important as 3D effects.”
REVIVAL OF THE STALLED CORE-COLLAPSE SUPERNOVA SHOCK TRIGGERED BY PRECOLLAPSE ASPHERICITY IN THE PROGENITOR STAR (2013, methodology): “We use the multispecies neutrino leakage scheme of O’Connor & Ott (2010), whose 3D version was also employed in Ott et al. (2012); Ott et al. (2013).”
The Status of Multi-Dimensional Core-Collapse Supernova Models (2016, unknown): “…light-bulb models) currently in use for 1D and multiD models include: • leakage schemes as, e.g., in O’Connor & Ott (2010), O’Connor & Ott (2011), Ott et al. (2013) and Couch & O’Connor (2014) • the isotropic diffusion source approximation (IDSA) of Liebendörfer et al. (2009), • one-moment…”
Characterizing the Gravitational Wave Signal from Core-collapse Supernovae (2018, background): “Second, the detection of correlated neutrino and GW temporal variability might provide a way to diagnose large-scale chaotic motion in the supernova core (Ott et al. 2012; Kuroda et al. 2017).”
THE LANDSCAPE OF THE NEUTRINO MECHANISM OF CORE-COLLAPSE SUPERNOVAE: NEUTRON STAR AND BLACK HOLE MASS FUNCTIONS, EXPLOSION ENERGIES, AND NICKEL YIELDS (2014, background): “…et al. 1995; Fryer & Heger 2000; Fryer & Warren 2002, 2004; Buras et al. 2006; Murphy & Meakin 2011; Burrows et al. 2012; Murphy et al. 2013; Ott et al. 2013), the standing accretion shock instability (SASI) and/or vortical-acoustic instability (Foglizzo 2002; Blondin et al. 2003; Blondin &…”
SASI ACTIVITY IN THREE-DIMENSIONAL NEUTRINO-HYDRODYNAMICS SIMULATIONS OF SUPERNOVA CORES (2013, methodology): “In contrast to the findings by Burrows et al. (2012); Murphy et al. (2012); Dolence et al. (2013) and by Ott et al. (2012), we observe strong SASI activity in our 3D simulations both for the 27M⊙ progenitor and the 25M⊙ star.”
What can be learned from a future supernova neutrino detection (2017, background): “Supernova explosion mechanics such as SASI are predicted to leave their imprint on not only neutrino [359, 360, 358, 111] but also gravitational wave [397, 398, 399, 128, 400, 401] time modulations; thus, cross correlations can yield more sensitive and robust probes.”
The Gravitational Wave Signal from Core-collapse Supernovae (2018, methodology): “Interestingly, our linear analysis presents an opportunity to predict the dominant frequency of the GWs from CCSNe based on 1D simulations.”