Presents a grid of 113 fast-rotating, chemically-homogeneous massive star models at Z=0.001 reaching core collapse with high angular momentum for use as supernova and GRB progenitors.
Core Collapse Supernova Modeling: The Next Ten Years
6 Pith papers cite this work. Polarity classification is still indexing.
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abstract
Core collapse supernova modeling has advanced considerably since the first numerical simulations were performed sixty years ago. In particular, the last decade has brought us sophisticated three-dimensional models with significant predictive capabilities -- e.g., for core collapse supernova gravitational wave emission. The six decades of modeling have shown us the importance of individual components of these general relativistic neutrino radiation magnetohydrodynamics events -- specifically, the importance of neutrino kinetics, fluid instabilities, magnetic fields, strong gravity, and the nuclear equation of state and neutrino--matter interactions calculated in a manner consistent with the equation of state. They have also shown us that simulation outcomes are sensitive to variations in the treatment of these ingredients, demanding a level of rigor that has not yet been consistently met by modelers. The efficacy of the neutrino shock reheating mechanism for core collapse supernovae has been demonstrated. The models now require an improved quantitative predictive capability, which will be achieved through increased sophistication in the treatment of model components, both macroscopic (e.g., strong-field gravity) and microscopic (e.g., neutrino--matter interactions). Advancement of core collapse supernova theory will also require the cooperation of modelers in other fields, especially stellar evolution and nuclear theory, to meet the level of rigor required to make the most of the eventuality of a Galactic core collapse supernova and its multimessenger emissions.
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contest 1representative citing papers
A southern circum-jet ring in the Crab Nebula is identified and attributed to a counterjet within the jittering-jets explosion mechanism framework.
A mean-field magnetic polytrope model shows radiation pressure can unbind an n=3 polytrope when the central overpressure exceeds roughly 0.15 times a mass-dependent factor under small radial perturbations.
Morphological similarity between JWST images of planetary nebula PMR 1 and X-ray images of CCSN remnant RCW 103 indicates that two pairs of jets shaped RCW 103, supporting the jittering-jets explosion mechanism.
Analysis of JWST observations identifies point-symmetric morphology in SNR 0540-69.3 ejecta, interpreted as evidence for shaping by at least three jet pairs in the jittering-jets explosion mechanism.
Morphological similarity between pipe features in PNe and CCSNRs and a jet simulation is used to argue that jets formed the pipes and to bolster the JJEM for core-collapse supernovae.
citing papers explorer
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A grid of fast-rotating, chemically-homogeneous, supernova and/or long-GRB progenitors
Presents a grid of 113 fast-rotating, chemically-homogeneous massive star models at Z=0.001 reaching core collapse with high angular momentum for use as supernova and GRB progenitors.
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Identifying a circum-jet southern ring counterpart to the northern jet of the Crab Nebula
A southern circum-jet ring in the Crab Nebula is identified and attributed to a counterjet within the jittering-jets explosion mechanism framework.
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Non-linear Dynamical Stability of Magnetic Polytropes
A mean-field magnetic polytrope model shows radiation pressure can unbind an n=3 polytrope when the central overpressure exceeds roughly 0.15 times a mass-dependent factor under small radial perturbations.
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JWST observations of a planetary nebula support jet-driven explosion of core-collapse supernova remnant RCW 103
Morphological similarity between JWST images of planetary nebula PMR 1 and X-ray images of CCSN remnant RCW 103 indicates that two pairs of jets shaped RCW 103, supporting the jittering-jets explosion mechanism.
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JWST observations support the jittering-jets explosion mechanism (JJEM) for the core-collapse supernova remnant SNR 0540-69.3
Analysis of JWST observations identifies point-symmetric morphology in SNR 0540-69.3 ejecta, interpreted as evidence for shaping by at least three jet pairs in the jittering-jets explosion mechanism.
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The jet-shaped pipe morphology in planetary nebulae and core-collapse supernova remnants
Morphological similarity between pipe features in PNe and CCSNRs and a jet simulation is used to argue that jets formed the pipes and to bolster the JJEM for core-collapse supernovae.