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Temperature structure of active regions deduced from the helium-like sulphur lines |
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| Authors: | Tetsuya Watanabe Hirohisa Haka Toshifumi Shimizu Eijiro Hiei Robert D. Bentley James Lang Kenneth J. H. Phillips C. David Pike Andrzej Fludra Barbara J. I. Bromage John T. Mariska |
| Affiliation: | (1) National Astronomical Observatory, 181 Mitaka, Tokyo, Japan;(2) Faculty of Science, University of Tokyo, 113 Bunkyo-ku, Japan;(3) Department of Physics, Meisei University, 191 Hino, Tokyo, Japan;(4) Mullard Space Science Laboratory, Holmbury St. Mary, RH5 6NT Surrey, U.K.;(5) Rutherford Appletown Laboratory, OX11 0QX Didcot, Oxon, U.K.;(6) Centre for Astrophysics, University of Central Lancashire, PR1 2HZ Preston, Lancs, U.K.;(7) Naval Research Laboratory, 23075 Washington, D.C., USA |
| Abstract: | Solar active-region temperatures have been determined from the full-Sun spectra of helium-like sulphur (Sxv) observed by the Bragg Crystal Spectrometer on board theYohkoh satellite. The average temperature deduced from Sxv is demonstrated to vary with the solar activity level: A temperature of 2.5 × 106 K is derived from the spectra taken during low solar activity, similar to the general corona, while 4 × 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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