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R. F. Stein, D. Bercik, D. Georgobiani (Michigan State Univ.), A. Nordlund (Teoretisk Astrofysik Center, DK)
Results from realistic simulations of near surface solar convection will be summarized and compared with observations.
Solar convection is driven by radiative cooling from an extremely thin surface thermal boundary layer, which produces low entropy fluid. Its topology is controlled by mass conservation and consists of turbulent downdrafts penetrating nearly laminar upflows. The horizontal scales increase with depth.
Good agreement is found with the of the depth of the convection zone, p-mode frequencies, excitation, line asymmetries and intensity - velocity phase differences from helioseismology; with observations of granulation and profiles of weak Fe lines.
This work was supported by grants from NSF, NASA, and the Danish Research Council. The calculations were performed at NCSA, MSU and UNI\bulletC.
If the author provided an email address or URL for general inquiries, it is a
s follows:
http://www.pa.msu.edu/~steinr/talks/conv99