We perform an unprecedented high-resolution simulation for the photo voltaic convection zone. Our calculation reproduces the quick equator and close to-surface shear layer (NSSL) of differential rotation and the near-surface poleward meridional movement simultaneously. The NSSL is situated in a posh layer where the spatial and time scales of thermal convection are significantly small compared with the deep convection zone. While there have been a number of makes an attempt to reproduce the NSSL in numerical simulation, the results are nonetheless removed from actuality. On this study, we achieve reproducing an NSSL in our new calculation. 4) the turbulent viscosity and magnetic tension are latitudinally balanced with the Coriolis force in the NSSL. We emphasize the importance of the magnetic discipline within the photo voltaic convection zone. ††software: R2D2 Hotta et al. The Sun is rotating differentially with the fast equator and the sluggish pole. Omega in the solar inside. Within the solar convection zone, we've got two shear layers, i.e., the tachocline round the base of the convection zone and the close to-surface shear layer (NSSL).

The tachocline is thought to be maintained by the interaction between the convection and radiation zones (Spiegel & Zahn, 1992