The new picture of the transition region and corona from SUMER

Details The new picture of the transition region and corona from SUMER The new picture of the transition region and corona from SUMER

Jun 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002esasp.508..531f&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

Physics

2

Solar Transition Region, Solar Corona

Scientific paper

The solar upper atmosphere (SUA) is defined as the volume above the photosphere occupied by plasmas at electron temperatures greater than 2×104K. Until the Skylab era, little was known about the morphology of the SUA. As a result, the early models assumed a continuous atmosphere in which the temperature increased with height. With the advances in spectroscopic measurements it became apparent that most of the radiation from plasmas at temperatures of 3×104 - 6×105K is not coming from the interface between the chromosphere and corona but rather from unrelated plasma structures that I chose to name Unresolved Fine Structures (UFS). Recent results obtained by instruments on SOHO and on TRACE support the earlier conclusions and provide additional insight into the makeup of the SUA plasma structures of quiet Sun and coronal-hole regions.

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