Solar prominences in the extreme ultraviolet as observed from the Apollo Telescope Mount

Details Solar prominences in the extreme ultraviolet as observed from the Apollo Telescope Mount Solar prominences in the extreme ultraviolet as observed from the Apollo Telescope Mount

Dec 1974

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1974soph...39..337s&link_type=abstract

Solar Physics, vol. 39, Dec. 1974, p. 337-347.

Physics

31

Apollo Telescope Mount, Far Ultraviolet Radiation, Line Spectra, Solar Prominences, Solar Spectra, Fine Structure, Lyman Alpha Radiation, Optical Thickness, Skylab Program, Solar Corona, Solar Limb, Spectroheliographs

Scientific paper

Observations of quiescent solar prominences with the Harvard College Observatory spectrometer aboard Skylab show that prominence material is optically thick in the Lyman alpha line and the Lyman continuum. The color temperature of the Lyman continuum has a mean of 6600 K and an upward gradient toward the top of the prominence. The departure coefficient of the ground state of hydrogen is found to be of the order of unity, as expected from theory. The optical depth of the C III sheath region is determined directly from the observation of the limb through the prominence and is used to infer the mean electron density and the temperature gradient of the sheath. The result implies that the sheath density is about 0.4, and the temperature gradient about 1.4 times the respective value in the C III transition zone of the quiet sun. The C III triplet-singlet ratio for the prominence is found to give a density compatible, within the uncertainty of the atomic parameters, with the density obtained from the optical depth.

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