Stellar Magnetic Structure and Activity
Stellar Magnetic Structure and Activity
复制标题
恒星的磁结构和活动
DOI：
10.1007/978-94-009-8479-0_25
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发表时间：
1981
期刊：
影响因子：
--
通讯作者：
C. Zwaan
中科院分区：
文献类型：
--
作者：
C. Zwaan
对冷恒星的磁结构和活动的研究在很大程度上受到太阳的启发。在太阳中，磁场集中在形成一个序列的离散元素中，从大的暗太阳黑子到磁网络中明亮的小元素。磁场强度的范围从太阳黑子本影的3千高斯到网络元素的1.5千高斯（有关评论，见Harvey，1977和Zwaan，1980）。这一序列可以用一组静磁通量管模型来解释，这些模型取决于通过管的磁通量（有关总结和参考文献，请参见Zwaan，1978）。静磁模型中的一个基本假设是磁通管内的能流不超过对流区能流的20%。
The study of magnetic structure and activity in cool stars is largely inspired by the Sun. In the Sun the magnetic field has been concentrated in discrete elements which form a sequence, from the large dark sunspots down to the bright small elements in the magnetic network. The field strengths range from 3 kilo-gauss in sunspot umbrae to about 1.5 kilogauss in the network elements (for reviews, see Harvey, 1977 and Zwaan, 1980). This sequence may be explained by a set of magnetostatic flux tube models which depend on the magnetic flux through the tube (for a summary and references, see Zwaan, 1978). A basic assumption in the magnetostatic modeling is that the energy flux within the flux tube is no more than 20% of the energy flux in the nonmagnetic convection zone.