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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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.
Late-time IR spectroscopy of SN 2024ggi shows varied line morphologies implying chemical inhomogeneity and aspherical ionization, with modeling favoring 12-15 solar mass progenitors but only high-mass energetic 3D simulations matching the observed Ni mixing extent.
Hydrodynamic simulations of three jet pairs in the jittering-jets mechanism reproduce the ring-and-bar morphology of supernova remnant G11.2-0.3.
No kilonova detected from sub-solar GW candidate S251112cm, but coincident IIb supernova SN 2025adtq yields suggestive evidence for the superkilonova channel, though inconclusive after accounting for chance coincidence.
N6946-BH1's remnant is roughly 10 times fainter than its progenitor while stellar merger remnants are 10-100 times brighter, and asymmetric dust cannot explain the difference.
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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Mapping 3-D Explosive Nucleosynthesis with Type II Supernova Infrared Emission Lines
Late-time IR spectroscopy of SN 2024ggi shows varied line morphologies implying chemical inhomogeneity and aspherical ionization, with modeling favoring 12-15 solar mass progenitors but only high-mass energetic 3D simulations matching the observed Ni mixing extent.
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Simulating the jittering-jets explosion mechanism: Supernova remnant G11.2-0.3
Hydrodynamic simulations of three jet pairs in the jittering-jets mechanism reproduce the ring-and-bar morphology of supernova remnant G11.2-0.3.
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Electromagnetic Follow-up of the Sub-Solar Mass Gravitational Wave Candidate S251112cm: Kilonova Constraints and a Coincident IIb Supernova
No kilonova detected from sub-solar GW candidate S251112cm, but coincident IIb supernova SN 2025adtq yields suggestive evidence for the superkilonova channel, though inconclusive after accounting for chance coincidence.
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The neighboring stars of N6946-BH1 and the observational characteristics of failed supernovae
N6946-BH1's remnant is roughly 10 times fainter than its progenitor while stellar merger remnants are 10-100 times brighter, and asymmetric dust cannot explain the difference.