Solar differential rotation reproduced with high-resolution simulation
Solar differential rotation reproduced with high-resolution simulation
复制标题
通过高分辨率模拟再现太阳差分旋转
DOI：
10.1038/s41550-021-01459-0
复制
发表时间：
2021
期刊：
影响因子：
14.1
通讯作者：
Kusano K.
中科院分区：
文献类型：
--
作者：
Hotta H.;Kusano K.
太阳以快赤道和慢极的方式进行差异旋转。太阳内部的对流被认为维持了差速旋转。然而，尽管已经进行了许多数值模拟来重现太阳差分自转， , , , – ，但之前对太阳参数的高分辨率计算属于反太阳（快极）差分自转范围。因此，我们仍然不知道太阳赤道快速旋转的真正原因。虽然快赤道的构建需要对对流产生强烈的旋转影响，但之前的计算无法在不进行任何操作的情况下实现这种情况。这个问题被称为对流难题。数值模拟中的对流和差动旋转与观测结果不同。在这里，我们展示了高分辨率计算成功地再现了类似太阳的差分旋转。我们的计算表明，小型发电机产生的强磁场对热对流有显着影响。在我们的计算中成功再现了差分旋转、对流和磁场，这是理解太阳活动最基本性质（特别是太阳黑子活动的 11 年周期）成因的重要一步。
The Sun rotates differentially with a fast equator and slow pole. Convection in the solar interior is thought to maintain the differential rotation. However, although many numerical simulations have been conducted to reproduce the solar differential rotation, , , , –, previous high-resolution calculations with solar parameters fall into the antisolar (fast-pole) differential rotation regime. Consequently, we still do not know the true reason why the Sun has a fast-rotating equator. While the construction of the fast equator requires a strong rotational influence on the convection, the previous calculations have not been able to achieve the situation without any manipulations. The problem is called the convective conundrum. The convection and the differential rotation in numerical simulations were different from the observations. Here, we show that a high-resolution calculation succeeds in reproducing the solar-like differential rotation. Our calculations indicate that the strong magnetic field generated by a small-scale dynamo has a significant impact on thermal convection. The successful reproduction of the differential rotation, convection and magnetic field achieved in our calculation is an essential step to understanding the cause of the most basic nature of solar activity, specifically, the 11 yr cycle of sunspot activity.