Other
Scientific paper
Jun 2002
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002esasp.508..237p&link_type=abstract
In: Proceedings of the SOHO 11 Symposium on From Solar Min to Max: Half a Solar Cycle with SOHO, 11-15 March 2002, Davos, Switze
Other
1
Sun: Transition Region, Sun: Corona, Stars: Coronae
Scientific paper
One of the keys to the understanding of coronal heating is the structure of the thin transition region from the chromosphere to the corona. All the energy that is ultimately heating the corona has to be transported somehow from the photosphere through this thin layer. As the "natural" time-scales are very small in the transition region the analysis of the EUV emission formed between 104 to 106K provides a suitable tool to study effects of the energy transport. As we are far from spatially resolving the transition region, spectroscopy can be used to deconvolve the emission from different structures. If either the line width or the line shift or both signatures differ, one can still study two regions even though they are not spatially resolved. This is especially true if the different structures are on top of each other ("vertically"). One example are large coronal funnels arching over smaller transition region loops. These spectroscopic techniques can also be used to interpret observations of stellar transition regions. This paper will try to give an overview of the various transition region structures and their physical nature, as well as on the required observational techniques.
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