Helioseismic Probing of Giant-Cell Convection

Details Helioseismic Probing of Giant-Cell Convection Helioseismic Probing of Giant-Cell Convection

Jun 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006spd....37.3201f&link_type=abstract

American Astronomical Society, SPD meeting #37, #32.01; Bulletin of the American Astronomical Society, Vol. 38, p.257

Astronomy and Astrophysics

Astronomy

1

Scientific paper

The turbulent solar convection zone exhibits a range of scales of convection which are visible at the solar surface, ranging from granules ( 1 Mm) to supergranules ( 30 Mm). Numerical simulations of solar convection carried out in full spherical shells consistently reveal even larger scales of convection, termed giant cells, which may span a few hundreds of Mm in the horizontal and extend over much of the convection zone. Recent correlation tracking of supergranular motions has revealed the tendency of supergranules to align themselves in the north-south direction. This alignment is possibly due to organization by larger-scale giant cell motions and is generally weak, with the strongest alignment occurring at the equator. Using f-mode time-distance and specialized averaging and tracking techniques, we probe for the possible flow signals associated with the presence of these giant cells near the solar equator.

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