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The relation between hot and cool loops

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Abstract

In order to study the origin of the hot (≳3 MK) corona above active regions, we compare Yohkoh/SXT X-ray images, which represent a broad temperature range above ∼ 2.5 MK, with TRACE EUV coronal images whose primary sensitivities are in the 1–2 MK range. Nearly simultaneous X-ray and EUV snapshots show that there are loops that appear similar in these images of different temperature sensitivities, but they are not exactly cospatial with each other. A significant difference is noted in the active region core, where bright loops are seen in X-ray images but not in EUV images, reflecting their high (∼5 MK) temperatures. In SXT time-sequence images, these loops are found to undergo repetitive minor brightenings, suggestive of their flare-like origin. This is consistent with the absence of the EUV counterparts of the X-ray loops in TRACE time-sequence images at earlier and later times. We need to revisit the validity of the assumption that coronal loops are steady.

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Nitta, N. The relation between hot and cool loops. Solar Physics 195, 123–133 (2000). https://doi.org/10.1023/A:1005251322006

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  • DOI: https://doi.org/10.1023/A:1005251322006

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