PERSISTENT MAGNETIC WREATHS IN A RAPIDLY ROTATING SUN

Journal Article · Mon Mar 01 00:00:00 EST 2010 · Astrophysical Journal

DOI:https://doi.org/10.1088/0004-637X/711/1/424· OSTI ID:21394355

Brown, Benjamin P; Toomre, Juri ^[1]; Browning, Matthew K ^[2]; Brun, Allan Sacha ^[3]

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1. JILA and Department of Astrophysical and Planetary Sciences, University of Colorado, Boulder, CO 80309-0440 (United States)
2. Canadian Institute for Theoretical Astrophysics, University of Toronto, Toronto, ON M5S3H8 (Canada)
3. DSM/IRFU/SAp, CEA-Saclay and UMR AIM, CEA-CNRS-Universite Paris 7, 91191 Gif-sur-Yvette (France)

When our Sun was young it rotated much more rapidly than now. Observations of young, rapidly rotating stars indicate that many possess substantial magnetic activity and strong axisymmetric magnetic fields. We conduct simulations of dynamo action in rapidly rotating suns with the three-dimensional magnetohydrodynamic anelastic spherical harmonic (ASH) code to explore the complex coupling between rotation, convection, and magnetism. Here, we study dynamo action realized in the bulk of the convection zone for a system rotating at 3 times the current solar rotation rate. We find that substantial organized global-scale magnetic fields are achieved by dynamo action in this system. Striking wreaths of magnetism are built in the midst of the convection zone, coexisting with the turbulent convection. This is a surprise, for it has been widely believed that such magnetic structures should be disrupted by magnetic buoyancy or turbulent pumping. Thus, many solar dynamo theories have suggested that a tachocline of penetration and shear at the base of the convection zone is a crucial ingredient for organized dynamo action, whereas these simulations do not include such tachoclines. We examine how these persistent magnetic wreaths are maintained by dynamo processes and explore whether a classical mean-field alpha-effect explains the regeneration of poloidal field. We find that the global-scale toroidal magnetic fields are maintained by an OMEGA-effect arising from the differential rotation, while the global-scale poloidal fields arise from turbulent correlations between the convective flows and magnetic fields. These correlations are not well represented by an alpha-effect that is based on the kinetic and magnetic helicities.

• OSTI ID: 21394355
• Journal Information: Astrophysical Journal, Vol. 711, Issue 1; Other Information: DOI: 10.1088/0004-637X/711/1/424; ISSN 0004-637X
• Country of Publication: United States
• Language: English

Related Subjects

30 DIRECT ENERGY CONVERSION
AXIAL SYMMETRY
CONVECTION
HELICITY
MAGNETIC FIELDS
MAGNETISM
MAGNETOHYDRODYNAMICS
MEAN-FIELD THEORY
ROTATION
SIMULATION
SUN
THREE-DIMENSIONAL CALCULATIONS
ENERGY TRANSFER
FLUID MECHANICS
HEAT TRANSFER
HYDRODYNAMICS
MAIN SEQUENCE STARS
MASS TRANSFER
MECHANICS
MOTION
PARTICLE PROPERTIES
STARS
SYMMETRY