Astronomy and Astrophysics – Astrophysics
Scientific paper
Dec 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufmsh42a..03w&link_type=abstract
American Geophysical Union, Fall Meeting 2010, abstract #SH42A-03
Astronomy and Astrophysics
Astrophysics
[7524] Solar Physics, Astrophysics, And Astronomy / Magnetic Fields, [7544] Solar Physics, Astrophysics, And Astronomy / Stellar Interiors And Dynamo Theory
Scientific paper
We use a thin flux tube model in a rotating spherical shell of turbulent convective flows computed separately from an existing 3D global simulation to study how active region scale flux tubes rise buoyantly from the bottom of the convection zone to near the solar surface. We investigate initial toroidal flux tubes at the base of the convection zone with field strengths ranging from 15 kG to 100 kG at initial latitudes ranging from 2 to 40 degrees. We find that the dynamic evolution of the flux tube changes from magnetic buoyancy dominated to convection dominated as we decrease the initial field strength from 100 kG to 15 kG. At 100 kG, the strong tension of the flux tube is able to resist the bending due to the convective flows and the development of Omega-shaped rising loops are mainly controlled by the growth of the magnetic buoyancy instability, with the strongest convective down drafts producing some moderate perturbations to the final emerging loops. The mean properties of the final emerging loops are in agreement with previous thin flux tube models in the absence of convection. On the other hand, at a low field strength of 15 kG, we find that the development of the rising Omega-shaped loops are largely controlled by the convective flows and the properties of the emerging loops are significantly changed compared to the results from previous thin flux tube models in the absence of convection. With convection, the rise times are drastically reduced (from years to 1-2 months), the loops are able to emerge at low latitudes, and the majority of the emerging loops show tilt angles of the proper sign (consistent with the active region tilts), and also show a field strength asymmetry that would be consistent with the observed morphological asymmetry of active regions. We discuss the implications of these results with regard to the field strength of the dynamo generated large-scale toroidal magnetic field at the base of the solar convection zone.
Fan Ying
Miesch Marck
Weber Mark A.
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