We perform an unprecedented excessive-resolution simulation for the photo voltaic convection zone. Our calculation reproduces the quick equator and near-surface shear layer (NSSL) of differential rotation and the near-floor poleward meridional flow simultaneously. The NSSL is positioned in a posh layer the place the spatial and time scales of thermal convection are significantly small compared with the deep convection zone. While there have been several makes an attempt to reproduce the NSSL in numerical simulation, the results are still removed from actuality. On this research, we achieve reproducing an NSSL in our new calculation. 4) the turbulent viscosity and magnetic tension are latitudinally balanced with the Coriolis pressure within the NSSL. We emphasize the importance of the magnetic area 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 bottom of the convection zone and the close to-surface shear layer (NSSL).

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