Simulation of large-scale flows at the solar surface

Details Simulation of large-scale flows at the solar surface Simulation of large-scale flows at the solar surface

Oct 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989apj...345.1060s&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 345, Oct. 15, 1989, p. 1060-1078. Research supported by the National Solar

Astronomy and Astrophysics

Astrophysics

25

Convection, Magnetohydrodynamic Flow, Solar Atmosphere, Solar Granulation, Analytic Functions, Continuity Equation, Plumes, Polarimeters, Spacelab, Velocity Distribution

Scientific paper

A simple analytic axisymmetric function is used to represent the radial outflow associated with an isolated convection plume at the solar surface. The vertical velocity can be deduced from the continuity equation. A regular cellular pattern of convection can be created by superposing a number of such sources. The function is applied to the large-scale horizontal motions observed by the Solar Optical Universal Polarimeter (SOUP) instrument on Spacelab 2. The flow pattern visible in three different regions covered by the SOUP observations is simulated. In each case a superposition of the plume functions mimics the observed mesogranular and supergranular motions well. The model flows are used to compute the motion of passive test particles (corks) which accumulate in a network that outlines mesogranular cells. Detailed comparisons suggest that magnetic flux tubes are affected more by outflow from sources at the centers of mesogranules than by flow into sinks within the network.

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