The fine structure of prominences. V - Active edges of quiescent prominences

Details The fine structure of prominences. V - Active edges of quiescent prominences The fine structure of prominences. V - Active edges of quiescent prominences

Nov 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978soph...60...57e&link_type=abstract

Solar Physics, vol. 60, Nov. 1978, p. 57-65.

Physics

13

Fine Structure, Line Spectra, Solar Activity, Solar Prominences, Solar Spectra, D Lines, Doppler Effect, Emission Spectra, K Lines, Solar Magnetic Field

Scientific paper

A significant number (at least one-third) of all quiescent prominences contain Doppler shifted features associated with their edges or emission gaps between prominence substructures. The individual spectral structures have lifetimes of 5-15 min, dimensions perpendicular to the edge of 1-2 arc sec, and may be lined along the visible edge of a prominence for distances up to 30 arc sec; velocities average 3-40 km/sec. The Ca II K, He I D3, and H-alpha line intensity ratios may be interpreted by a slightly higher temperature than average for the prominence. The possibility that the features represent ejecta expelled at the local Alfven speed from a heated current sheet is considered.

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