The fine structure of the solar atmosphere in the far ultraviolet

Details The fine structure of the solar atmosphere in the far ultraviolet The fine structure of the solar atmosphere in the far ultraviolet

Sep 1974

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1974soph...38..133b&link_type=abstract

Solar Physics, vol. 38, Sept. 1974, p. 133-156.

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Astronomical Photography, Far Ultraviolet Radiation, Fine Structure, Solar Atmosphere, Solar Corona, Spectroheliographs, Filtergrams, High Resolution, Polar Caps, Rocket Sounding, Solar Limb, Solar Spectra, Spectral Resolution, Spicules, Sunspots

Scientific paper

The paper describes qualitatively the spatial distribution of UV emission obtained from high resolution spectroheliograms in the UV emission lines He I, He II, O IV, O V, and Ne VII photographed during a sounding rocket flight. Broad band filtergrams of the far UV solar corona were also obtained. The results confirmed that spicules are the location of UV emission. Most of the UV emission in the temperature range from 100,000 to 200,000 K is concentrated in and around the spicules and this concentration decreases with increasing temperatures. Four different areas of UV emission are discussed. The He I and He II spectroheliogram observations showed He to be suppressed in the coronal holes, polar caps, and sunspots.

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