Physics
Scientific paper
Aug 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006iaujd..17e...6r&link_type=abstract
Highlights of Recent Progress in the Seismology of the Sun and Sun-Like Stars, 26th meeting of the IAU, Joint Discussion 17, 23
Physics
Scientific paper
We present a non-kinematic, flux-transport dynamo model for the S un that combines a mean - field model for differential rotation and meridional flow with the mean - field induction equation. The induced magnetic field is allowed to feed back on differential rotation and meridional flow through the macroscopic Lorentz force, leading to solar cycle variations of zonal and meridional flows. We show that the dynamo saturates through this feedback at a field strength of around 10 - 2 0 kG and that the equator ward transport of field by the meridional flow at the base of the convection zone (essential for flux-transport dynamos) is not significantly reduced. The non-linear dynamo is capable of explaining the high- latitude branch of torsional oscillations (having correct amplitude and phase relation with respect to the magnetic butterfly diagram), but cannot explain the low- latitude branch through macroscopic Lorentz-force feedback. We present a compound model that includes a parameterisation of enhanced radiative losses in the active region belt (following the idea of Spruit 2003, Solar Physics 213, 1) and show that this can provide the correct oscillation pattern in low latitudes close to the surface. Thermally- driven inflows into the active region belt produced by this model are also consistent with observations.
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