Physical conditions in the solar atmosphere above an active region

Details Physical conditions in the solar atmosphere above an active region Physical conditions in the solar atmosphere above an active region

Aug 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980apj...240..300m&link_type=abstract

Astrophysical Journal, Part 1, vol. 240, Aug. 15, 1980, p. 300-305. NASA-supported research.

Physics

Atomic Physics

12

Solar Activity, Solar Atmosphere, Solar Corona, Solar Spectra, Electron Density (Concentration), Emission Spectra, Extreme Ultraviolet Radiation, Line Spectra, Ultraviolet Spectra

Scientific paper

From a series of EUV spectra obtained at several heights above the limb in a solar active region, the volume emission measure is derived as a function of the electron temperature in the temperature range 70,000-1,500,000 K and the electron density at two locations. The emission measure from the coronal material (temperature greater than 700,000 K) is nearly the same everywhere and represents most of the material in the line of sight, while the emission measure from the transition region material (temperature between 70,000 and 250,000 K) fluctuates by two orders of magnitude from position to position above the active region. This is in agreement with the picture of this active region as consisting of a number of well-defined loops or lower portions of loops at transition region temperatures that are inhomogeneously distributed in much larger and more diffuse loop structures at coronal temperatures. The coronal data are in reasonable agreement with simple coronal models. Emission measures near 1,000,000 K evaluated using different ions differ by a factor of 4, suggesting difficulties with the atomic physics data.

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