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.
Astronomy and Astrophysics , author=
3 Pith papers cite this work, alongside 23 external citations. Polarity classification is still indexing.
3
Pith papers citing it
23
external citations · OpenAlex
fields
astro-ph.SR 3years
2026 3verdicts
UNVERDICTED 3representative 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.
Slowly rotating 80–85 M☉ Pop III stars can keep most of their mass and form black holes with spins up to a_BH ≲ 0.7 just below the pair-instability gap.
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.
-
Fast-spinning massive black holes from slowly rotating low-metallicity stars: Implications for GW231123
Slowly rotating 80–85 M☉ Pop III stars can keep most of their mass and form black holes with spins up to a_BH ≲ 0.7 just below the pair-instability gap.