We present a set of numerical simulations that model the convection zones of solar-like stars. With this suite of numerical experiments, we explore how the nature of the convective structures transitions through a series of morphological regimes as the reduced Rayleigh number increases. Convection first manifests as a belt of rotationally aligned, convective, Taylor columns that circumscribes the equator. As the supercriticality increases, the poles begin to convect, initially in a cellular form, but eventually a plumy form emerges. Finally, at extremely high values of the Rayleigh number, a weakly rotating regime is achieved with antisolar differential rotation, i.e., the equator rotates more slowly than the poles. For all of these regimes, we provide theoretical and empirical scaling relations that summarize how global quantities—such as the bulk Rossby number and Reynolds number—scale with the Rayleigh and Ekman numbers. We demonstrate that a Rossby number based on the proper...

中文翻译：

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旋转星对流型态的形态分类

我们提出了一组数值模拟，模拟了太阳般恒星的对流区。通过这套数值实验，我们探索了随着瑞利数的减少，对流结构的性质如何通过一系列形态学形态过渡。对流首先表现为围绕赤道的旋转对准的对流泰勒柱带。随着超临界度的增加，两极开始对流，最初以蜂窝形式对流，但最终出现了羽状形式。最后，在瑞利数极高的值下，通过反太阳差速旋转实现了弱旋转，即赤道旋转的速度比磁极旋转的速度慢。对于所有这些制度，我们提供了理论和经验的比例关系，这些关系总结了总体数量（例如，大块Rossby数和雷诺数）如何与Rayleigh和Ekman数成比例。我们证明基于适当的...的罗斯比数