Heat flow near obstacles in the solar convection zone

Details Heat flow near obstacles in the solar convection zone Heat flow near obstacles in the solar convection zone

Nov 1977

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1977soph...55....3s&link_type=abstract

Solar Physics, vol. 55, Nov. 1977, p. 3-34.

Physics

Condensed Matter

Superconductivity

95

Convective Flow, Heat Transmission, Solar Physics, Thermal Diffusion, Turbulent Diffusion, Diffusion Coefficient, Mixing Length Flow Theory, Stellar Models, Sunspots, Superconductivity, Thermal Conductivity

Scientific paper

A turbulent thermal diffusion coefficient based on a mixing length approximation is used to analyze the behavior of inhomogeneities in the heat flow in the solar convection zone. The analysis models the convection zone as a thermally superconducting shell enclosed between a thin surface layer and an interior of low thermal conductivity. Inhomogeneities within the convection zone create only weak sunspots unless they are nearer than 2000 km to the surface. Calculations taking into account the very high conductivity of convecting matter show that the heat flux blocked below a sunspot spreads over a wide area surrounding the spot, which may explain the 'missing flux problem'.

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