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+<br>We perform an unprecedented excessive-decision simulation for the photo voltaic convection zone. Our calculation reproduces the quick equator and close to-floor shear layer (NSSL) of differential rotation and the close to-floor poleward meridional circulate simultaneously. The NSSL is located in a posh layer the place the spatial and time scales of thermal convection are considerably small compared with the deep convection zone. While there have been a number of attempts to reproduce the NSSL in numerical simulation, the results are nonetheless far from reality. On this study, we succeed in 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 importance of the magnetic discipline in the solar convection zone. ††software: R2D2 Hotta et al. The Sun is rotating differentially with the fast equator and the gradual pole. Omega in the solar interior. Within the photo voltaic convection zone, now we have two shear layers, i.e., the tachocline round the bottom of the convection zone and the near-floor shear layer (NSSL).<br>
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+<br>The tachocline is thought to be maintained by the interplay between the convection and radiation zones (Spiegel & Zahn, 1992
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