Simulation of the Sun's Differential Rotation and Magnetic Field

太阳的磁场是由太阳对流层中的发电机作用产生的，可能是在该层的深处和辐射内部顶部的过冲区域。 发电机机制是强烈的对流区，这本身在很大程度上是由雷诺应力与湍流内的差分旋转的影响。 PI将开发一个新的太阳能发电机和太阳对流区内的差动旋转模拟。 为此，他将进一步发展必要的湍流传输理论，以通过全球模拟中无法解决的湍流尺度来解释磁场，动量和熵的平均通量。 为了验证和完成理论，他将在代表太阳内部不同深度和纬度的控制体积中进行对流磁湍流的数值模拟。 当获得湍流的稳健参数化后，他将在差分旋转和平均太阳磁场的全球模拟中使用它。

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.