Astronomy and Astrophysics – Astrophysics
Scientific paper
Dec 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufmsh42a..02r&link_type=abstract
American Geophysical Union, Fall Meeting 2010, abstract #SH42A-02
Astronomy and Astrophysics
Astrophysics
[7524] Solar Physics, Astrophysics, And Astronomy / Magnetic Fields, [7529] Solar Physics, Astrophysics, And Astronomy / Photosphere, [7544] Solar Physics, Astrophysics, And Astronomy / Stellar Interiors And Dynamo Theory
Scientific paper
The flux emergence process transporting magnetic field from the solar interior into the photosphere and beyond is central to our understanding of solar magnetism. However, due to the wast range of length and time scales as well as different physical regimes encountered from the base of the solar convection zone to the solar corona, a fully coherent picture of this process does not yet exist. In this talk I review models addressing the flux emergence within the bulk of the convection zone as well as models of the last stages of flux emergence and active region formation in the upper most 10-20 Mm of the convection zone and photopshere. I will discuss the prospects of coupling these models in the near future. The latter had been hampered in the past primarily by the fact that realistic MHD simulations of the upper convection zone and photosphere were restricted to rather small domains compared to the typical scale of an active region. Over that past 5 years a combination of advancement in numerical methods and high performance computing has enabled numerical simulations on the scale of entire sunspots with sufficient resolution to capture the essence of sunspot fine structure. Currently these simulations are expanded even further to the scale of active regions to address the flux emergence process and active region formation in the photosphere. The National Center for Atmospheric Research is sponsored by the National Science Foundation. This work is in part supported by the NASA SDO Science Center.
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