Morphological Classification of the Convective Regimes in Rotating Stars
Morphological Classification of the Convective Regimes in Rotating Stars
复制标题
旋转恒星对流体系的形态分类
作者：
B. Hindman;N. Featherstone;K. Julien
我们提出了一组模拟类太阳恒星对流区的数值模拟。通过这一套数值实验，我们探索了对流结构的性质是如何随着减少的瑞利数的增加而通过一系列形态制度转变的。对流首先表现为沿赤道旋转排列的对流泰勒柱带。随着超临界的增加，两极开始对流，最初以细胞形式出现，但最终出现羽状形式。最后，在极高的瑞利数值下，反太阳微分旋转达到弱旋转状态，即赤道比两极旋转得慢。对于所有这些制度，我们提供了理论和经验尺度关系，总结了整体数量-如体积罗斯比数和雷诺数-与瑞利和埃克曼数的尺度关系。我们证明，基于附着在对流区外表面的热边界层性质的罗斯比数特别适用于预测向反太阳微分旋转的转变。
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 properties of the thermal boundary layer that clings to the outer surface of the convection zone works particularly well to predict the transition to antisolar differential rotation.
登录
查看更多内容
高瑞利数球形对流中的普朗特数效应
DOI：
10.3847/1538-4357/aaaeb5
发表时间：
2018
期刊：
The Astrophysical Journal
影响因子：
--
作者：
Orvedahl, Ryan J.;Calkins, Michael A.;Featherstone, Nicholas A.;Hindman, Bradley W.
通讯作者：
Hindman, Bradley W.
影响因子：
4.8
作者：
Gastine, T.;Yadav, R. K.;Wicht, J.
通讯作者：
Wicht, J.
影响因子：
3.2
作者：
Gastine, T.;Wicht, J.
通讯作者：
Wicht, J.
影响因子：
3.2
作者：
Jones, C. A.;Boronski, P.;Wicht, J.
通讯作者：
Wicht, J.