A MAP OF THE HORIZONTAL FLOWS IN THE SOLAR CONVECTION ZONE

The first map of the horizontal flows as a function of depth and heliocentric position in the solar convection zone is presented. The map is inferred from a least-squares smoothness-constrained inversion of velocities measured from ring diagrams of the solar p-mode oscillations. The data provide information in four longitude regions at a latitude just south of the solar equator. The presence of several features is suggested by the results: (1) A prograde directed longitudinal jet between the hydrogen and first helium ionization zone, reversing direction to retrograde below the second helium ionization zone. (2) A equatorward directed latitudinal flow above the second helium ionization zone. (3) A poleward latitudinal flow below the second helium ionization zone, but only in one of the four longitude bands. A large active region was present in this band, but not in two of the other bands, suggesting a possible relationship between the activity and the different flow pattern. The magnitude of the flows is substantial, reaching some 450 m s-1 for the longitudinal jet, and 150 m s-1 for the latitudinal flow. Possible systematic errors and the physical consequences of the flows are discussed. © 1990 Kluwer Academic Publishers.