The Structure of the Static Corona and Transition Region
The Structure of the Static Corona and Transition Region
复制标题
静态电晕和过渡区的结构
DOI：
10.1086/163912
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发表时间：
1986
期刊：
影响因子：
--
通讯作者：
G. Noci
中科院分区：
文献类型：
--
作者：
S. Antiochos;G. Noci
研究了冕环的静态模型。对于低海拔的色球层以上的高度低于约5000公里的环路，它示出了一种新的类型的解决方案出现的静态方程，除了著名的日冕环路解决方案。新解决方案的特征在于最大等离子体温度小于约100，000K。这些冷溶液的结构和性质进行了讨论。计算了磁拱廊的差分发射测量Q（T），它必须自然地包含热回路和冷回路。结果表明，冷环对下过渡区Q（T）的形式有显著的影响。特别是，它们可以解释在低T下观察到的Q上升，这一直被认为与静态环路模型不相容。最后，讨论了冷环对太阳和恒星日冕和过渡区的其他观测的影响。
Static models of coronal loops are investigated. For loops that are low-lying with heights above the chromosphere below about 5000 km, it is shown that a new type of solution appears to the static equations, in addition to the well-known coronal loop solution. The new solution is characterized by a maximum plasma temperature less than about 100,000 K. The structure and properties of these cool solutions are discussed. The differential emission measure Q(T) expected for a magnetic arcade, which must naturally contain both hot and cool loops, is calculated. It is shown that the cool loops have a dramatic effect on the form of Q(T) in the lower transition region. In particular, they can account for the observed rise in Q at low T, which has long been thought to be incompatible with the static-loop model. Finally, the implications of the cool loops on other observations of both the solar and stellar coronae and transition regions are discussed.