Convective structures in the sun

Details Convective structures in the sun Convective structures in the sun

Sep 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991mnras.252p...1s&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 252, Sept. 1, 1991, p. 1P-5P. Research supported by SER

Astronomy and Astrophysics

Astronomy

25

Convection Currents, Photosphere, Solar Granulation, Solar Magnetic Field, Angular Momentum, Plumes, Radiative Heat Transfer

Scientific paper

Observed patterns of motion at the solar surface reflect the structure of subphotospheric convection, which controls the distribution of angular momentum and magnetic fields. Mesogranules are interpreted as secondary features associated with supergranular circulation, and that coupling between mesogranules and granulation triggers the spasmodic formation of exploding granules. Supergranules are expected to generate isolated sinking plumes. It is argued that these plumes can penetrate to the base of the convective zone, and that there is no organized structure on larger scales.

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