Physics
Scientific paper
Aug 1975
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975soph...43..327f&link_type=abstract
Solar Physics, vol. 43, Aug. 1975, p. 327-336.
Physics
99
Magnetic Field Configurations, Pressure Distribution, Solar Activity, Solar Magnetic Field, Solar Temperature, Temperature Distribution, Far Ultraviolet Radiation, H Alpha Line, K Lines, Line Spectra, Lines Of Force, Lyman Alpha Radiation, Magnetic Flux, Plasma Density, Solar Atmosphere, Ultraviolet Spectra
Scientific paper
EUV observations show many active region loops in lines formed at temperatures between 10,000 and 2,000,000 K. The brightest loops are associated with flux tubes leading to the umbrae of sunspots. It is shown that the high visibility of certain loops in transition region lines is due principally to a sharp radial decrease of temperature to chromospheric values toward the loop axis. The plasma density of these cool loops is not significantly greater than in the hot gas immediately surrounding it. Consequently, the internal gas pressure of the cool material is clearly lower. The hot material immediately surrounding the cool loops is generally denser than the external corona by a factor 3-4. When the active region is examined in coronal lines, this hot high pressure plasma shows up as loops that are generally parallel to the cool loops but significantly displaced laterally.
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