By Hideyuki Hotta
This thesis describes the reports at the sunlight inside the place turbulent thermal convection performs a tremendous function. the writer solved, for the 1st time, one of many long-standing concerns in sunlight physics, i.e., the upkeep mechanism of the sun differential rotation within the near-surface shear layer. the writer attacked this challenge with a newly constructed procedure, the diminished velocity of sound procedure, which enabled him to enquire the skin and deep sun layers in a self-consistent demeanour. this method additionally made it attainable to accomplish an remarkable functionality within the sunlight convection simulations for the use of the vastly parallel supercomputers akin to the RIKEN okay approach. It used to be discovered that the turbulence and the suggest flows similar to the differential rotation and the meridional move jointly engage with one another to keep up the stream buildings within the sunlight. fresh observations by means of helioseismology help the author's proposed theoretical mechanism. The publication additionally addresses the new release of the magnetic box in such turbulent convective motions, that is an incredible leap forward for sun cyclic dynamo research.
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Extra info for Thermal Convection, Magnetic Field, and Differential Rotation in Solar-type Stars
15 a The correlation between the radial velocity and the strength of the magnetic field ( vr , B ), b the horizontal average of the generation rate of the magnetic energy by the stretching ( Wstr : solid lines) and the compression ( Wcmp : dashed lines), c the correlation between the radial velocity and the generation rate of the magnetic energy ( vr , Wstr ), d the correlation between the strength of the magnetic field and the generation rate of the magnetic energy ( B, Wstr ) are shown A, B = ABd S A2 d S B2d S .
We use δθ = 3Δθ/2 and δφ = 3Δφ/2 for the interpolation with the third-order function, where Δθ and Δφ are the grid spacings in latitudinal and longitudinal directions. Although the boundary condition for the Yin grid is applied on the edge of the Yin grid, the boundary condition for the Yang grid is applied on the edge of the Yin grid to avoid the double solution in the overlapping area of the Yin-Yang grid (Fig. 3). The red thick lines show the location of the horizontal boundary for both Yin and Yang grids.
The integrated fluxes show almost the similar behavior as those in the case H0, but the maximum absolute values of the enthalpy and kinetic flux are smaller. Since these absolute values gradually decrease from H0 to H2, we conclude that both the thickness of the cooling layer and the location of the upper boundary contribute to this issue. It is possible that, when the upper boundary becomes closer to the real solar surface and the cooling layer becomes thinner, the absolute values of the enthalpy flux and kinetic flux become even larger than our case H0.