Coronal loops are the building blocks of the solar atmosphere. Un-derstanding their mechanism of formation means understanding the mechanism responsible for heating the solar corona. The properties of coronal loops are only partially established. Several issues such as the relationship among structures seen at different temperatures, the temperature distribution of the emission, or the degree of filamentation within a volume remain under discussion. Hinode, as the new generation solar observatory, provides the best suited diagnostics to address some of these issues. We demonstrate that this is the case using a case study, AR 10978, and encourage systematic studies of larger samples as solar activity increases. Results for AR 10978 are consistent with loops rooted in highly dynamic unipolar magnetic field areas made of multiple strands that get heated to at least 2.5 MK, and cool down rather coherently to transition region temperatures.
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机译：冠状环是太阳能大气的构建块。不受他们的形成机制意味着了解负责加热太阳能电晕的机制。冠状环的性质仅部分建立。在不同温度下看到的结构之间的关系，发射温度分布的几个问题，或体积内的细丝的程度仍然存在讨论。作为新一代太阳天文台的Hinode提供了最适合解决这些问题的最适合的诊断。我们证明了这种情况，使用案例研究，AR 10978，并促进随着太阳能活性的增加，较大样本的系统研究。 AR 10978的结果与由多个股线制成的高动态单极磁场区域的环，该循环源于多条股线，该围绕至少2.5mK加热至至少2.5 mk，并且在过渡区域温度下冷却。
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