Physics
Scientific paper
Jan 1982
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982soph...75..189d&link_type=abstract
Solar Physics, vol. 75, Jan. 1982, p. 189-203.
Physics
56
Coronal Loops, Extreme Ultraviolet Radiation, Hydrostatics, Solar Activity, Solar Magnetic Field, Spectroheliographs, Electron Density (Concentration), Fine Structure, Line Spectra, Photosphere, Skylab Program, Solar Corona, Spaceborne Photography
Scientific paper
XUV spectroheliograms of two active regions are used to illustrate the structure of transition zone and coronal emissions. The observations were made with a XUV spectroheliograph aboard Skylab. Basically, the instrument consists of a single concave grating which focuses and disperses images of the sun onto photographic film. The film is located near the grating normal in order to minimize aberrations. It was found that XUV emission in active regions is produced mainly in either loops or network. Lines formed above 1,000,000 K are formed solely in loop structures while lines below that temperature are formed in the network and in loops or loop segments. The hot loops generally end in regions of enhanced transition zone emissions (network) which are well correlated with photospheric magnetic fields. The cooler loops also end in network regions and are not always associated with sunspots. This agrees with conclusions of Cheng (1980).
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