Stellar Chromospheric Activity
Stellar Chromospheric Activity
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DOI：
10.12942/lrsp-2008-2
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发表时间：
2008-03
影响因子：
20.9
通讯作者：
Jeffrey C. Hall
中科院分区：
文献类型：
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作者：
Jeffrey C. Hall
太阳、与它相似的恒星以及许多与它很不相同的恒星都有色球层。色球层通常被视为位于明亮的光球层之上，其特征是具有正的温度梯度以及明显偏离辐射平衡。恒星色球层呈现出各种各样的现象，这些现象统称为活动，主要源于它们磁场的时间演化以及通过复杂的磁拓扑结构和恒星外层大气中越来越光学薄的等离子体的质量通量和辐射传输。在这篇综述中，我将（1）概述从1960年至今我们对色球层结构的认识发展，（2）讨论主要的观测项目和理论研究方向，（3）综述太阳和恒星色球层活动的起源和性质，以及它与包括总能量输出在内的恒星参数的关系和对其的影响，（4）总结当今悬而未决的问题。
The Sun, stars similar to it, and many rather dissimilar to it, have chromospheres, regions classically viewed as lying above the brilliant photosphere and characterized by a positive temperature gradient and a marked departure from radiative equilibrium. Stellar chromospheres exhibit a wide range of phenomena collectively called activity, stemming largely from the time evolution of their magnetic fields and the mass flux and transfer of radiation through the complex magnetic topology and the increasingly optically thin plasma of the outer stellar atmosphere. In this review, I will (1) outline the development of our understanding of chromospheric structure from 1960 to the present, (2) discuss the major observational programs and theoretical lines of inquiry, (3) review the origin and nature of both solar and stellar chromospheric activity and its relationship to, and effect on, stellar parameters including total energy output, and (4) summarize the outstanding problems today.