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首页> 外文期刊>Philosophical transactions of the Royal Society. Mathematical, physical, and engineering sciences >What can observations tell us about coronal heating?
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What can observations tell us about coronal heating?

机译：观测可以告诉我们关于冠状动脉加热的什么？

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摘要

The actual source of coronal heating is one of the longest standing unsolved mysteries in all of astrophysics, but it is only in recent years that observations have begun making significant contributions. Coronal loops, their structure and sub-structure, their temperature and density details, and their evolution with time, may hold the key to solving this mystery. Because spatial resolution of current observatories cannot resolve fundamental scale lengths, information about the heating of the corona must be inferred from indirect observations. Loops with unexpectedly high densities and multi-thermal cross-field temperatures were not consistent with results expected from steady uniform heating models. The hot (T > 5 MK) plasma component of loops may also be a key observation; a new sounding rocket instrument called the Marshall Grazing Incidence X-ray Spectrometer will specifically target this observable. Finally, a loop is likely to be a tangle of magnetic strands. The High Resolution Coronal Imager observed magnetic braids untwisting and reconnecting, dispersing enough energy to heat the surrounding plasma. The existence of multi-thermal, cooling loops and hot plasma provides observational constraints that all viable coronal heating models will need to explain.
机译：日冕加热的实际来源是所有天体物理学中存在时间最长的未解之谜之一，但是直到最近几年，观测才开始做出重大贡献。日冕环，其结构和子结构，其温度和密度的详细信息以及它们随时间的演变，可能是解决这个谜题的关键。由于当前天文台的空间分辨率无法解析基本尺度长度，因此必须从间接观测中推断出有关电晕加热的信息。具有异常高密度和多热交叉场温度的回路与稳定均匀加热模型所预期的结果不一致。回路的热（T> 5 MK）等离子体成分也可能是关键观察点;一种称为马歇尔放牧入射X射线光谱仪的新型探空火箭仪器将专门针对此可观测物体。最后，回路很可能是磁链的缠结。高分辨率日冕成像仪观察到磁性编织带解开并重新连接，分散了足够的能量来加热周围的等离子体。多热，冷却回路和热等离子体的存在提供了所有可行的日冕加热模型都需要解释的观测约束。

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