Institute for Solar Physics of the Royal Swedish Academy of Sciences, and Department of Astronomy at Stockholm University, AlbaNova University Center, SE-10691 Stockholm, Sweden.
Science. 2011 Jul 15;333(6040):316-9. doi: 10.1126/science.1206429. Epub 2011 Jun 2.
The fine structure and dynamics of sunspots and the strong outflow in their outer filamentary part--the penumbra--have puzzled astronomers for more than a century. Recent theoretical models and three-dimensional numerical simulations explain the penumbral filaments and their radiative energy output as the result of overturning convection. Here, we describe the detection of ubiquitous, relatively dark downward flows of up to 1 kilometer per second (km/s) in the interior penumbra, using imaging spectropolarimetric data from the Swedish 1-meter Solar Telescope. The dark downflows are omnipresent in the interior penumbra, distinguishing them from flows in arched flux tubes, and are associated with strong (3 to 3.5 km/s) radial outflows. They are thus part of a penumbral convective flow pattern, with the Evershed flow representing the horizontal component of that convection.
太阳黑子的精细结构和动力学以及其外部丝状部分（半影）中的强外流，令天文学家困惑了一个多世纪。最近的理论模型和三维数值模拟将半影细丝及其辐射能量输出解释为对流翻转的结果。在这里，我们使用来自瑞典 1 米太阳望远镜的成像光谱偏振数据，描述了在内部半影中普遍存在的、速度高达 1 公里每秒（km/s）的相对较暗的向下流动的检测结果。这些暗的下降流在内部半影中普遍存在，将它们与弓形通量管中的流动区分开来，并与强烈的（3 到 3.5km/s）径向外流相关联。因此，它们是半影对流模式的一部分，埃vershed 流代表了该对流的水平分量。
