Some structural features of the convective-velocity field in the solar photosphere

Details Some structural features of the convective-velocity field in the solar photosphere Some structural features of the convective-velocity field in the solar photosphere

Mar 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010arep...54..254g&link_type=abstract

Astronomy Reports, Volume 54, Issue 3, pp.254-259

Astronomy and Astrophysics

Astronomy

1

Scientific paper

An algorithm for measuring horizontal photospheric velocities previously employed to process aerospace images is adapted for problems in solar physics and realized in a computational code. It differs from the standard procedure of local correlation tracking in a special choice of trial areas (“targets”), whose displacements are determined bymaximizing the correlation between the original and various shifted positions of the target. Specifically, an area is chosen as a target in a certain neighborhood of each node of a predefined grid if either the contrast or the entropy of the brightness distribution reaches its maximum in this area. The horizontal velocities obtained are then interpolated to the positions of imaginary “corks” using the Delaunay triangulation and affine transformations specified by the deformation of the obtained triangles at the time step considered. The motion of the corks is represented by their trajectories. A superposition of flows on different scales, from mesogranular to supergranular, can clearly be seen. “Large mesogranules” with sizes of order 15 Mm are revealed. In many cases, these are stellate in shape. Areas of strong convergence of the horizontal flows are detected; this convergence is sometimes accompanied by swirling. Evidence is found for the possible coexistence of convection cells with different circulation directions, so-called l-type and g-type cells.

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