In a 3D MHD simulation, the near-core magnetic field at the convective-radiative boundary is toroidally dominated and the rotational shear layer is confined to the Brunt-Väisälä peak, contradicting the dipolar assumption in magneto-asteroseismology.
I., & MiMeS Collaboration
1 Pith paper cite this work. Polarity classification is still indexing.
1
Pith paper citing it
citation-role summary
background 1
citation-polarity summary
fields
astro-ph.SR 1years
2024 1verdicts
CONDITIONAL 1roles
background 1polarities
background 1representative citing papers
citing papers explorer
-
On the Geometry of the Near-Core Magnetic Field in Massive Stars
In a 3D MHD simulation, the near-core magnetic field at the convective-radiative boundary is toroidally dominated and the rotational shear layer is confined to the Brunt-Väisälä peak, contradicting the dipolar assumption in magneto-asteroseismology.