The coronal and transition region temperature structure of a solar active region

Details The coronal and transition region temperature structure of a solar active region The coronal and transition region temperature structure of a solar active region

May 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980soph...66...39l&link_type=abstract

Solar Physics, vol. 66, May 1980, p. 39-60. Research supported by the Science Research Council;

Astronomy and Astrophysics

Astronomy

15

Electron Energy, Emission Spectra, Far Ultraviolet Radiation, Solar Corona, Solar Temperature, Ultraviolet Spectra, X Ray Spectra, Apollo Telescope Mount, Data Processing, Electron Density (Concentration), Skylab Program, Solar Spectra, Solar Wind, Spaceborne Astronomy, Spectroheliographs, Transition Temperature

Scientific paper

Using measurements of EUV and X-ray spectral lines, the differential emission measure vs electron temperature from the transition region to the corona of an active region (electron temperature between 100,000 and 5,000,000 K) is derived. The total emission measure and radiative losses are of the order 3 x 10 to the 48th/cu cm and 4 x 10 to the 26th ergs/sec, respectively. The emission measure at electron temperatures greater than approximately 1,000,000 K (i.e. that mainly responsible for the X-ray emission) is about 75% of the total. The use of the Mg x line at 625 A as an indicator of coronal electron density is also examined. A set of theoretical energy balance models of coronal loops in which the loop divergence is a variable parameter is presented and compared with the observations.

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