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We perform an unprecedented high-resolution simulation for the solar convection zone. Our calculation reproduces the fast equator and close to-surface shear layer (NSSL) of differential rotation and the near-floor poleward meridional flow concurrently. The NSSL is situated in a posh layer the place the spatial and time scales of thermal convection are considerably small in contrast with the deep convection zone. While there have been a number of attempts to reproduce the NSSL in numerical simulation, the results are still removed from actuality. On this examine, we succeed in reproducing an NSSL in our new calculation. 4) the turbulent viscosity and magnetic tension are latitudinally balanced with the Coriolis force within the NSSL. We emphasize the importance of the magnetic subject in the photo voltaic convection zone. ††software: R2D2 Hotta et al. The Sun is rotating differentially with the quick equator and the slow pole. Omega within the photo voltaic inside. Within the solar convection zone, we now have two shear layers, i.e., the tachocline around the base of the convection zone and the close to-surface shear layer (NSSL). https://dev.neos.epss.ucla.edu/wiki/index.php?title=Must_You_Choose_Double-Cut_Shears_Or_Single-Cut_Shears