3D MHD simulations of pre-supernova Wolf-Rayet progenitors reveal cylindrical rotation and amplified small-scale magnetic fields that connect regions isolated in 1D models.
M., Chatzopoulos , E., Arnett , W
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3D MHD simulations of pre-supernova progenitors find turbulent mixing in oxygen and silicon shells deviates from standard 1D mixing-length prescriptions, with proposed updates for stellar evolution codes.
The authors implement and validate nuclear networks coupled to GRRMHD with M1 neutrino transport in Gmunu, showing effects on core-collapse supernova shock revival and composition.
2D core-collapse supernova simulations of 15 solar-mass progenitors with varied multi-D initial structures show similar explosion dynamics, with no detectable impact from progenitor turbulence due to saturation by post-shock instabilities.
citing papers explorer
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The first 3D MHD core-collapse progenitors II: Rotation, magnetic-field amplification, and magnetic topology
3D MHD simulations of pre-supernova Wolf-Rayet progenitors reveal cylindrical rotation and amplified small-scale magnetic fields that connect regions isolated in 1D models.
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The first 3D MHD core-collapse progenitors I: General properties, convection and nuclear burning
3D MHD simulations of pre-supernova progenitors find turbulent mixing in oxygen and silicon shells deviates from standard 1D mixing-length prescriptions, with proposed updates for stellar evolution codes.
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Toward First-Principles Multi-Messenger Predictions: Coupling Nuclear Networks with GR Radiation-MHD in {\tt Gmunu}
The authors implement and validate nuclear networks coupled to GRRMHD with M1 neutrino transport in Gmunu, showing effects on core-collapse supernova shock revival and composition.
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Impacts of Multidimensional Progenitor Perturbations on Core-Collapse Supernova Explosions
2D core-collapse supernova simulations of 15 solar-mass progenitors with varied multi-D initial structures show similar explosion dynamics, with no detectable impact from progenitor turbulence due to saturation by post-shock instabilities.