Temperature structure of active regions deduced from helium-like sulphur lines

Details Temperature structure of active regions deduced from helium-like sulphur lines Temperature structure of active regions deduced from helium-like sulphur lines

Mar 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995soph..157..169w&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 157, no. 1-2, p. 169-184

Physics

22

Solar Activity, Solar Physics, Solar Spectra, Solar Temperature, Sulfur, Sun, Emission Spectra, Emissivity, Solar Corona

Scientific paper

Solar active-region temperatures have been determined from the full-Sun spectra of helium-like sulfur (S XV) observed by the Bragg Crystal Spectrometer on Board the Yohkoh satellite. The average temperature deduced from S XV is demonstrated to vary with the solar activity level: A temperature of 2.5 x 106 K is derived from the spectra taken during low solar activity, similar to the general corona, while 4 x 106 K is obtained during a higher activity phase. For the latter, the high- temperature tail of the differential emission measure of active regions is found most likely due to the superposition of numerous flare-like events (micro/nano-flares).

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