We perform an unprecedented high-resolution simulation for the solar convection zone. Our calculation reproduces the quick equator and Wood Ranger Power Shears near-surface shear layer (NSSL) of differential rotation and the near-floor poleward meridional stream simultaneously. The NSSL is positioned in a complex 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 attempts to reproduce the NSSL in numerical simulation, the outcomes are nonetheless far from reality. In this research, we reach 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 discipline 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 solar interior. In the solar convection zone, we've two shear layers, i.e., the tachocline round the bottom of the convection zone and the near-floor shear layer (NSSL).
The tachocline is thought to be maintained by the interaction between the convection and radiation zones (Spiegel & Zahn, 1992