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We carry out an unprecedented high-resolution simulation for the solar convection zone. Our calculation reproduces the quick equator and close to-floor shear layer (NSSL) of differential rotation and the close to-surface poleward meridional movement concurrently. The NSSL is situated in a complex layer the place the spatial and time scales of thermal convection are significantly small in contrast with the deep convection zone. While there have been several attempts to reproduce the NSSL in numerical simulation, the outcomes are still far from actuality. On this examine, we reach 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 importance of the magnetic subject in the solar convection zone. ††software: R2D2 Hotta et al. The Sun is rotating differentially with the quick equator and the sluggish pole. Omega in the photo voltaic inside. Within the photo voltaic convection zone, we now have two shear layers, i.e., the tachocline round the base of the convection zone and the close to-floor shear layer (NSSL).
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