We perform an unprecedented high-decision simulation for the solar convection zone. Our calculation reproduces the fast equator and near-surface shear layer (NSSL) of differential rotation and the close to-floor poleward meridional movement concurrently. The NSSL is positioned in a complex layer where the spatial and time scales of thermal convection are considerably small in contrast with the deep convection zone. While there have been several attempts to reproduce the NSSL in numerical simulation, the results are nonetheless far from actuality. In 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 in the NSSL. We emphasize the significance of the magnetic field within the solar convection zone. ††software: R2D2 Hotta et al. The Sun is rotating differentially with the fast equator and the gradual pole. Omega within the photo voltaic inside. In the solar convection zone, we've got two shear layers, i.e., the tachocline around the bottom 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, Wood Ranger Power Shears 1992