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.
Title resolution pending
5 Pith papers cite this work, alongside 97 external citations. Polarity classification is still indexing.
5
Pith papers citing it
97
external citations · OpenAlex
citation-role summary
background 1
citation-polarity summary
years
2026 5roles
background 1polarities
background 1representative citing papers
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.
For a low-mass CCSN progenitor, rotation alone weakly and non-monotonically affects explosion energy and observables; only the fastest spin yields T/|W| spiral modes and spin-kick alignment, with core spin amplified by ~4000.
SLSN 2021bnw is best fit by a core-collapse explosion of a star with initial mass at least 61 solar masses, ejecta of 15-22.5 solar masses containing 1.7 solar masses of nickel-56 and 4 foe energy colliding with 7 solar masses of circumstellar matter.
Simulations show the low-T/|W| instability develops robustly across five nuclear EOS in a rapidly rotating 35 M⊙ progenitor, with dominant GW frequency correlating to PNS compactness and stiffness.
citing papers explorer
-
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.
-
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.
-
Effects of Rotation on 3D Core-Collapse Supernova Models for Low-Mass Progenitors
For a low-mass CCSN progenitor, rotation alone weakly and non-monotonically affects explosion energy and observables; only the fastest spin yields T/|W| spiral modes and spin-kick alignment, with core spin amplified by ~4000.
-
Helium superluminous SN 2021bnw : an explosion of a massive star with a pre-outburst
SLSN 2021bnw is best fit by a core-collapse explosion of a star with initial mass at least 61 solar masses, ejecta of 15-22.5 solar masses containing 1.7 solar masses of nickel-56 and 4 foe energy colliding with 7 solar masses of circumstellar matter.
-
Impact of the equation of state on core collapse supernovae I: the low-$T/|W|$ instability
Simulations show the low-T/|W| instability develops robustly across five nuclear EOS in a rapidly rotating 35 M⊙ progenitor, with dominant GW frequency correlating to PNS compactness and stiffness.