The 3D Nature of Convective Dynamos

Type Journal Article
Names M. Miesch, B. Brown, N. Nelson, M. Browning, A. S. Brun, J. Toomre
Publication AGU Fall Meeting Abstracts
Volume 23
Pages 01
Date December 1, 2011
Library Catalog NASA ADS
Abstract Solar observations throughout the extended minimum between cyles 23 and 24 have highlighted the intrinsically three-dimensional (3D) nature of the solar magnetic field. These include prominent multipolar components and low-latitude coronal holes observed with STEREO, asymmetric surface flux distributions in photospheric magnetograms, ond global, multi-scale magnetic linkages revealed by SDO. Axisymmetric mean-field dynamo models cannot capture this complexity, which ultimately arises from turbulent convection. The solar dynamo is a convective dynamo; convection is clearly responsible for the diversity of solar magnetic activity we observe, generating and organizing magnetic fields both directly by turbulent induction and indirectly via mean flows and MHD instabilities. Simulations of convective dynamos reveal the 3D nature of how large-scale magnetic fields are generated and provide insight into the intricate topology of the solar magnetic field, apparent even during solar minimum. I will describe recent work on the role of helicity and shear in magnetic self-organization and promising first steps toward linking convective dynamos with flux emergence.
Tags AND ASTRONOMY / Magnetic fields, AND ASTRONOMY / Solar activity cycle, AND ASTRONOMY / Solar and stellar variability, AND ASTRONOMY / Stellar interiors and dynamo theory, ASTROPHYSICS, [7524] SOLAR PHYSICS, [7536] SOLAR PHYSICS, [7537] SOLAR PHYSICS,
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