Other
Scientific paper
Oct 1999
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999esasp.446..229c&link_type=abstract
8th SOHO Workshop: Plasma Dynamics and Diagnostics in the Solar Transition Region and Corona. Proceedings of the Conference hel
Other
4
Scientific paper
An analysis of the modified SOHO/EIT as well as TRACE, and Yohkoh/SXT heliograms with a restricted range of intensities reveals that the large-scale (comparable with the solar disk diameter) emitting chains, discovered before on the Nobeyama Radioheliograph maps at 17 GHz, are also characteristic of EUV, soft X-ray and other ranges. It turns out that rather often the EUV and soft X-ray bright points and elements are not scattered chaotically through the solar disc, but are aligned at definite lines forming large-scale thin chains and threads of various (sometimes very puzzling) configurations. The reality of this novel phenomenon is confirmed by the fact that the form and location of the chains coincide on different SOHO and TRACE images in several EUV lines as well as in the soft X-ray and other ranges. The chains and threads display a strong evolution at the time scale of hours. Similar to the microwave chains, the EUV and soft X-ray chains and threads seem to be related to coronal mass ejections (CMEs). In particular, a spectacular evolution of the chains and threads appears to occur not only after a CME at the stage of the prolonged post-CME energy release, but also before that, when large-scale magnetic structures approach to their unstable state. An existence of these chains and threads appears to mean that some large-scale structures light as a result of the reconnection and energy release associated either with the long-term evolution of the large-scale magnetic fields or with disturbances identified with CME events. In particular, it is highly probable that the detected chains light separators and quasi-separatrix layers forming on the boundaries of different interacting large-scale magnetic flux systems in the united, complex and global solar magnetosphere.
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