How far can minimal models explain the solar cycle?

Abstract

A physically consistent model of magnetic field generation by convection in a rotating spherical shell with a minimum of parameters is applied to the Sun. Despite its unrealistic features the model exhibits a number of properties resembling those observed on the Sun. The model suggests that the large scale solar dynamo is dominated by a non-axisymmetric $m=1$ component of the magnetic field.

Accepted for publication in the Astrophysical Journal on 2012/01/30

References in corpus (4)

• Turbulent magnetic Prandtl number and magnetic diffusivity quenching from simulations
• Prandtl number dependence of convection driven dynamos in rotating spherical fluid shells
• Bistability and hysteresis of dipolar dynamos generated by turbulent convection in rotating spherical shells
• Relations between dynamo-region geometry and the magnetic behavior of stars and planets

Cited by in corpus (8)

• Stochastic Gravitational Wave Backgrounds
• Dipolar versus multipolar dynamos: the influence of the background density stratification
• What controls the magnetic geometry of M dwarfs?
• Helicity inversion in spherical convection as a means for equatorward dynamo wave propagation
• Dynamo Effects Near The Transition from Solar to Anti-Solar Differential Rotation
• Effects of shell thickness on cross-helicity generation in convection-driven spherical dynamos
• Differential rotation in convecting spherical shells with non-uniform viscosity and entropy diffusivity
• A study of global magnetic helicity in self-consistent spherical dynamos