Supergranulation Scale Convection Simulations

Details Supergranulation Scale Convection Simulations Supergranulation Scale Convection Simulations

Dec 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aspc..415...63s&link_type=abstract

The Second Hinode Science Meeting: Beyond Discovery-Toward Understanding ASP Conference Series, Vol. 415, proceedings of a meeti

Astronomy and Astrophysics

Astronomy

1

Scientific paper

Results of realistic simulations of solar surface convection on the scale of supergranules (48 and 96 Mm wide by 20 Mm deep) are presented. The simulations include the hydrogen, first and most of the second helium ionization zones. Horizontal magnetic field is advected into the domain by upflows at the bottom. Upflows stretch the field lines upward, while downflows push them down, thus producing loop like magnetic structures. The mass mixing length is 1.8 scale heights. Two thirds of the area is upflowing fluid except very close to the surface. The internal (ionization) energy flux is the largest contributor to the convective flux for temperatures less than 40,000 K and the thermal energy flux is the largest contributor at higher temperatures. The data is available for evaluating local helioseismic procedures.

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