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Meridional Flows, Differential Rotation, and Leptocline in 3D Radiative Hydrodynamics Simulations and Observations

Presentation #502.03 in the session Solar Interior Flow and Dynamics.

Published onSep 18, 2023
Meridional Flows, Differential Rotation, and Leptocline in 3D Radiative Hydrodynamics Simulations and Observations

Understanding the structuring and dynamics of the solar convection in the presence of the rotation is crucial for our understanding of the coupling of the turbulent convective motions and the large-scale dynamics, in particular, problems related to solar activity, such as the formation of differential rotation, meridional circulation, and self-organizations processes of the multi-scale convection. We analyze realistic 3D radiative hydrodynamics simulations of solar subsurface dynamics in the presence of rotation in a local domain 80 Mm wide and 25 Mm deep, located at different latitudes: the equator, 30 degrees, 60 degrees, and the Northern pole. The simulation results reveal the development of a shallow 10-Mm deep substructure of the Near-Surface Shear Layer (NSSL), characterized by a strong radial, rotational gradient and self-organized meridional flows. This shallow layer (“leptocline”) located in the hydrogen ionization zone is associated with enhanced anisotropic overshooting-type flows into a less unstable layer between the H and HeII ionization zones. We discuss current observational evidence of the leptocline, show how the radial variations of the differential rotation and meridional flow profiles vary with latitude, and present a comparison with helioseismic and surface observations. This work is supported by the NASA Heliophysics Supporting Research Program and NASA COFFIES DRIVE Center project.

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