Flux-dominated solar dynamo model with a thin shear layer

Abstract

Flux-dominated solar dynamo models have demonstrated to reproduce the main features of the large scale solar magnetic cycle, however the use of a solar like differential rotation profile implies in the the formation of strong toroidal magnetic fields at high latitudes where they are not observed. In this work, we invoke the hypothesis of a thin-width tachocline in order to confine the high-latitude toroidal magnetic fields to a small area below the overshoot layer, thus avoiding its influence on a Babcock-Leighton type dynamo process. Our results favor a dynamo operating inside the convection zone with a tachocline that essentially works as a storage region when it coincides with the overshoot layer.

4 pages, 2 figures, accepted for publication in Astronomische Nachrichten

References in corpus (5)

• The case for a distributed solar dynamo shaped by near-surface shear
• Full--Sphere Simulations of a Circulation--Dominated Solar Dynamo: Exploring the Parity Issue
• Numerical Simulations of Penetration and Overshoot in the Sun
• Kinematic solar dynamo models with a deep meridional flow
• How does the shape and thickness of the tachocline affect the distribution of the toroidal magnetic fields in the solar dynamo?

Cited by in corpus (5)

• Turbulent magnetic pumping in a Babcock-Leighton solar dynamo model
• MHD instabilities in accretion disks and their implications in driving fast magnetic reconnection
• The role of diffusivity quenching in flux-transport dynamo models
• Mean-field solar dynamo models with strong meridional flow at the bottom of the convection zone
• Delayed Babcock-Leighton dynamos in the diffusion-dominated regime