We carry out 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 near-surface poleward meridional circulation concurrently. The NSSL is located in a posh 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 makes an attempt to reproduce the NSSL in numerical simulation, the results are still removed from reality. In this study, we reach 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 significance of the magnetic area in 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 solar interior. Within the photo voltaic convection zone, we now have two shear layers, i.e., the tachocline around the base of the convection zone and the near-floor shear layer (NSSL).

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