The relation between hot and cool loops

Details The relation between hot and cool loops The relation between hot and cool loops

Jul 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000soph..195..123n&link_type=abstract

Solar Physics, v. 195, Issue 1, p. 123-133 (2000).

Physics

9

Scientific paper

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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