EUV observations of the same prominence at the limb and on the disk

Details EUV observations of the same prominence at the limb and on the disk EUV observations of the same prominence at the limb and on the disk

Jun 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002esasp.508..291c&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

Prominences, Filaments, Euv Lines

Scientific paper

The same prominence has been observed, using the Coronal Diagnostic Spectrometer (CDS) onboard the SOHO Satellite, at the eastern limb and, ten days later, on the disk as a filament. The intensity of the Transition Region lines above the prominence at the limb varies from 0.2 to 0.5 that of the Quiet Sun, depending on the line formation temperature, while the same quantity measured above the disk filament results negligible. The lack of emission observed in coronal lines above the filament indicates that the gas in between the Hα thin threads must be the hot coronal plasma. In this framework the observed difference between filament and prominence line intensity is ascribed to the different view angle of the thin tube-like transition region which must be present around each cool thread.

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