| 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 |
| URL |
http://adsabs.harvard.edu/abs/2011AGUFMSH23D..01M |
| 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, |