Simulation of the Sun's Differential Rotation and Magnetic Field

太阳的磁场是由太阳对流区的发电机作用产生的，可能在该层的深处和辐射内部顶部的过冲区域。发电机机制受到对流区内差动旋转的强烈影响，对流区差动旋转本身在很大程度上是由与湍流相关的雷诺应力驱动的。PI将开发一种新的模拟太阳发电机和太阳对流区内的差异旋转。为此，他将进一步发展湍流输运理论，以解释在全球模拟中无法分辨的湍流尺度下的磁场、动量和熵的平均通量。为了验证和完善这一理论，他将对代表太阳内部不同深度和纬度的控制体中的对流磁湍流进行数值模拟。当获得了湍流的可靠参数后，他将使用它来对差分旋转和平均太阳磁场进行全球模拟。

The Sun's magnetic field is created by dynamo action in the solar convection zone, probably deep within that layer and in the overshoot region at the top of the radiative interior. The dynamo mechanism is strongly affected by the differential rotation within the convection zone, which itself is largely driven by Reynolds stresses associated with the turbulence. The PI will develop a new simulation of the solar dynamo and the differential rotation within the solar convection zone. For this, he will further develop the turbulent transport theory necessary to explain the mean fluxes of magnetic field, momentum and entropy by the scales of turbulence that are unresolvable in global simulations. To validate and complete the theory, he will perform numerical simulations of convective magneto-turbulence in control volumes representing various depths and latitudes of the solar interior. When a robust parameterization of the turbulence has been obtained, he will use it in a global simulation of the differential rotation and the mean solar magnetic field.