Since we Use Non-linear Artificial Diffusion
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We perform an unprecedented excessive-resolution simulation for the solar convection zone. Our calculation reproduces the quick equator and near-floor shear layer (NSSL) of differential rotation and the near-surface poleward meridional circulate concurrently. The NSSL is positioned in a posh layer where the spatial and time scales of thermal convection are considerably small compared with the deep convection zone. While there have been several attempts to reproduce the NSSL in numerical simulation, the results are still 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 within the NSSL. We emphasize the significance of the magnetic subject within the solar convection zone. ††software: R2D2 Hotta et al. The Sun is rotating differentially with the fast equator and the slow pole. Omega within 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 near-floor shear layer (NSSL).


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