Topology of convection beneath the solar surface

Details Topology of convection beneath the solar surface Topology of convection beneath the solar surface

Jul 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989apj...342l..95s&link_type=abstract

Astrophysical Journal, Part 2 - Letters (ISSN 0004-637X), vol. 342, July 15, 1989, p. L95-L98. Research supported by the Carlsbe

Astronomy and Astrophysics

Astrophysics

281

Convection, Solar Atmosphere, Solar Granulation, Entropy, Hydrodynamic Equations, Radiant Heating, Surface Layers, Topology, Velocity Distribution

Scientific paper

It is shown that the topology of convection beneath the solar surface is dominated by effects of stratification. Convection in a strongly stratified medium has: (1) gentle expanding structureless warm upflows and (2) strong converging filamentary cool downdrafts. The horizontal flow topology is cellular, with a hierarchy of cell sizes. The small density scale height in the surface layers forces the formation of the solar granulation, which is a shallow surface phenomenon. Deeper layers support successively larger cells. The downflows of small cells close to the surface merge into filamentary downdrafts of larger cells at greater depths, and this process is likely to continue through most of the convection zone. Radiative cooling at the surface provides the entropy-deficient material which drives the circulation.

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