Supergranules as Probes of the Sun's Meridional Circulation
  Recent analysis revealed that supergranules (convection cells seen at the Sun's surface) are advected by the zonal flows at depths equal to the widths of the cells themselves. Here we probe the structure of the meridional circulation by cross-correlating maps of the Doppler velocity signal using a series of successively longer time lags between maps. We find that the poleward meridional flow decreases in amplitude with time lag and reverses direction to become an equatorward return flow at time lags > 24 hours. These cross-correlation results are dominated by larger and deeper cells at longer time lags. (The smaller cells have shorter lifetimes and do not contribute to the correlated signal at longer time lags.) We determine the characteristic cell size associated with each time lag by comparing the equatorial zonal flows measured at different time lags with the zonal flows associated with different cell sizes from a Fourier analysis. This association gives a characteristic cell size of ~50 Mm at a 24 hour time lag. This indicates that the poleward meridional flow returns equatorward at depths > 50 Mm -- just below the base of the surface shear layer. A substantial and highly significant equatorward flow (4.6 +/- 0.4 m/s) is found at a time lag of 28 hours corresponding to a depth of ~70 Mm. This represents one of the first positive detections of the Sun's meridional return flow and illustrates the power of using supergranules to probe the Sun's internal dynamics. 
David H. Hathaway
astro-ph.SR