Kavli Affiliate: Robert Cameron
| First 5 Authors: Adam J. Finley, Sacha A. Brun, Antoine Strugarek, Robert Cameron,
| Summary:
For Sun-like stars, the generation of toroidal magnetic field from poloidal
magnetic field is an essential piece of the dynamo mechanism powering their
magnetism. Previous authors have estimated the net toroidal flux generated in
each hemisphere of the Sun by exploiting its conservative nature. This only
requires observations of the surface magnetic field and differential rotation.
We explore this approach using a 3D magnetohydrodynamic dynamo simulation of a
cool star, for which the magnetic field generation is known throughout the
entire star. Changes to the net toroidal flux in each hemisphere were evaluated
using a closed line integral bounding the cross-sectional area of each
hemisphere, following the application of Stokes-theorem to the induction
equation; the individual line segments corresponded to the stellar surface,
base, equator, and rotation axis. The influence of the large-scale flows, the
fluctuating flows, and magnetic diffusion to each of the line segments was
evaluated, along with their depth-dependence. In the simulation, changes to the
net toroidal flux via the surface line segment typically dominate the total
line integral surrounding each hemisphere, with smaller contributions from the
equator and rotation axis. The bulk of the toroidal flux is generated deep
inside the convection zone, with the surface observables capturing this due to
the conservative nature of the net flux. Surface magnetism and rotation can
therefore be used to estimate the net toroidal flux generated in each
hemisphere, allowing us to constrain the reservoir of magnetic flux for the
next magnetic cycle. However, this methodology cannot identify the physical
origin, nor the location, of the toroidal flux generation. In addition, not all
dynamo mechanisms depend on the net toroidal field produced in each hemisphere,
meaning this method may not be able to characterise every magnetic cycle.
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