The helicity constraint in spherical shell dynamos

Abstract

The motivation for considering distributed large scale dynamos in the solar context is reviewed in connection with the magnetic helicity constraint. Preliminary accounts of 3-dimensional direct numerical simulations (in spherical shell segments) and simulations of 2-dimensional mean field models (in spherical shells) are presented. Interesting similarities as well as some differences are noted.

4 pages, 5 fig, proceedings of 5th Potsdam Thinkshop on Meridional flow, differential rotation, solar and stellar activity, to be published in Astron. Nachr

References in corpus (5)

• Global-Scale Turbulent Convection and Magnetic Dynamo Action in the Solar Envelope
• The case for a distributed solar dynamo shaped by near-surface shear
• Dynamo Action in the Solar Convection Zone and Tachocline: Pumping and Organization of Toroidal Fields
• Turbulent magnetic Prandtl number and magnetic diffusivity quenching from simulations
• Magnetic helicity effects in astrophysical and laboratory dynamos

Cited by in corpus (6)

• Small-scale magnetic helicity losses from a mean-field dynamo
• The asymmetry of sunspot cycles and Waldmeier relations as due to nonlinear surface-shear shaped dynamo
• Effects of Penetrative Convection on Solar Dynamo
• Advances in theory and simulations of large-scale dynamos
• Shear-driven and diffusive helicity fluxes in alpha-Omega dynamos
• Long-term Evolution of Large-scale Magnetic Fields in Rotating Stratified Convection