类太阳恒星的快速自转、活跃对流巢和全球尺度流
Rapid Rotation, Active Nests of Convection and Global-scale Flows in Solar-like Stars
摘要：
在太阳对流区，旋转与强烈的湍流对流耦合，形成全球尺度的差异旋转和纬向环流。我们的太阳在过去一定旋转得更快，正如许多快速旋转的年轻太阳型恒星的观测所表明的那样。在这里，我们探讨更快的旋转对流的模式，在这样的恒星和全球规模的流量是自洽建立的影响。在这些系统中的对流是丰富的时间依赖性，在我们最快速旋转的太阳中，出现了引人注目的空间局部对流模式。在这些系统中，赤道附近的对流主要是由一个或两个局部增强对流的补丁，在最高的旋转速率之间几乎是静止的流动。这些活跃的对流巢尽管体积小，但仍保持着很强的差异旋转。差速旋转的结构在我们所有的快速旋转的太阳中是相似的，具有快速的赤道和较慢的极点。我们发现，总剪切差旋转，作为测量纬度角速度对比度，三角洲_欧米茄，增加更快速的旋转，而相对剪切，三角洲_欧米茄/欧米茄，减少。相反，在更快速的旋转，纬向环流减少的能量和峰值速度，并打破成多个单元的环流在半径和纬度。
英文摘要：
In the solar convection zone, rotation couples with intensely turbulent convection to build global-scale flows of differential rotation and meridional circulation. Our sun must have rotated more rapidly in its past, as is suggested by observations of many rapidly rotating young solar-type stars. Here we explore the effects of more rapid rotation on the patterns of convection in such stars and the global-scale flows which are self-consistently established. The convection in these systems is richly time dependent and in our most rapidly rotating suns a striking pattern of spatially localized convection emerges. Convection near the equator in these systems is dominated by one or two patches of locally enhanced convection, with nearly quiescent streaming flow in between at the highest rotation rates. These active nests of convection maintain a strong differential rotation despite their small size. The structure of differential rotation is similar in all of our more rapidly rotating suns, with fast equators and slower poles. We find that the total shear in differential rotation, as measured by latitudinal angular velocity contrast, Delta_Omega, increases with more rapid rotation while the relative shear, Delta_Omega/Omega, decreases. In contrast, at more rapid rotation the meridional circulations decrease in both energy and peak velocities and break into multiple cells of circulation in both radius and latitude.
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