Supernova simulations from a 3D progenitor model - Impact of perturbations and evolution of explosion properties

By Bernhard Müller, T. Melson, Alexander Heger, Hideko Nomura Queen's University Belfast, M. University, Max Planck Institute for Astrophysics, U. Minnesota, S. University. 2017

214 citations recorded by the source corpus.

We study the impact of large-scale perturbations from convective shell burning on the core-collapse supernova explosion mechanism using three-dimensional (3D) multi-group neutrino hydrodynamics simulations of an 18 solar mass progenitor. Seed asphericities in the O shell, obtained from a recent 3D model of O shell burning, help trigger a neutrino-driven explosion 330ms after bounce whereas the shock is not revived in a model based on a spherically symmetric progenitor for at least another 300ms. We tentatively infer a reduction of the critical luminosity for shock revival by ~20% due to pre-collapse perturbations. This indicates that convective seed perturbations play an important role in the explosion mechanism in some progenitors. We follow the evolution of the 18 solar mass model into the explosion phase for more than 2s and find that the cycle of accretion and mass ejection is still ongoing at this stage. With a preliminary value of 0.77 Bethe for the diagnostic explosion energy, a baryonic neutron star mass of 1.85 solar masses, a neutron star kick of ~600km/s and a neutron star spin period of ~20ms at the end of the simulation, the explosion and remnant properties are slightly atypical, but still lie comfortably within the observed distribution. Although more refined simulations and a larger survey of progenitors are still called for, this suggests that a solution to the problem of shock revival and explosion energies in the ballpark of observations are within reach for neutrino-driven explosions in 3D.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/1774fe436cf87a09b65a7ef06b472adedd1bac1e

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Citations in the corpus

A successful 3D core-collapse supernova explosion model (2018, methodology): “Similar energy growth rates are found for the 3D simulations in the literature (see, e.g. Müller et al. 2017) and necessitate continuing 3D simulations for several seconds.”
Characterizing the Gravitational Wave Signal from Core-collapse Supernovae (2018, background): “We also plan to extend this work with the study of progenitors with moderate rotation and with relic perturbations from advanced nuclear burning stages (Couch et al. 2015; Müller et al. 2017), and to explore the GW signal over longer timescales.”
The overarching framework of core-collapse supernova explosions as revealed by 3D fornax simulations (2019, background): “…studies leading to collapse that reveal mixing processes, gravity waves, and dynamics that the problematic mixing-length prescription for convection can not capture (Couch et al. 2015; Jones et al. 2016; Chatzopoulos et al. 2016; Müller et al. 2017, 2018; Jones et al. 2019; Yoshida et al. 2019).”
The Gravitational Wave Signal from Core-collapse Supernovae (2018, background): “…of CCSNe with stateof-the-art neutrino physics have been recently performed by a number of groups (Melson et al. 2015b,a; Lentz et al. 2015; Müller et al. 2017; Ott et al. 2017; see also Takiwaki et al. 2012; Ott et al. 2013; Takiwaki et al. 2014; Müller 2015; Roberts et al. 2016; Pan et…”
Three-dimensional simulations of neutrino-driven core-collapse supernovae from low-mass single and binary star progenitors (2018, methodology): “In particular, uncertainties in the electron fraction Ye translate into an uncertainty in the composition of the iron group ejecta made by (partial) recombination of the neutrino-processed ejecta as discussed previously in Müller et al. (2017a).”
Exploring Fundamentally Three-dimensional Phenomena in High-fidelity Simulations of Core-collapse Supernovae (2018, background): “CCSN mechanism simulations with this progenitor (Müller et al. 2017) showed a dramatic impact from the realistic 3D progenitor, yielding a successful explosion for a case in which the comparable 1D progenitor failed.”
Science case for the Einstein telescope (2019, background): “The three-flavor neutrino flux emanating from the proto-neutron star could power itself a core collapse supernova via neutrino heating on delayed timescales of order one second [104–116].”