YOHKOH/WBS Recalibration and a Comprehensive Catalogue of Solar Flares Observed by YOHKOH SXT, HXT and WBS Instruments |
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| Authors: | J Sato Y Matsumoto K Yoshimura S Kubo J Kotoku S Masuda M Sawa K Suga M Yoshimori T Kosugi T Watanabe |
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| Institution: | (1) Department of Physics, Montana State University, Bozeman, MT, 59717-3840;(2) STE Laboratory, Nagoya University, 3-13 Honohara, Toyokawa, 442-8507, Aichi;(3) Department of Physics, University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, 113-0033 Tokyo;(4) Present address: MELCO Inc., 325 Kami-Machiya, Kamakura, 247-8250 Kanagawa, Japan;(5) Institute of Space and Astronautical Science, 3-1-1 Yoshinodai, Sagamihara, 229-8510, Kanagawa;(6) Kwasan Observatory, Omine-cho, Kitakazan, Yamashina-ku, 607-8471, Kyoto;(7) National Astronomical Observatory, 2-21-1 Osawa, Mitaka, 181-8588 Tokyo;(8) Department of Physics, Saint Paul's University, 3-34-1 Nishi-Ikebukuro, Toshima-ku, 171-8501 Tokyo |
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| Abstract: | The flare catalogue of the Yohkoh mission is compiled and linked to this article as an electronic supplement. For showing flare characteristics over wide energy
range concisely, we provide the images of Hard X-ray Telescope (HXT) and the Soft X-ray Telescope (SXT), and the spectra of
Hard X-ray Spectrometer (HXS) and Gamma-Ray Spectrometer (GRS) with the Wide Band Spectrometer (WBS) time profiles. The energy
versus pulse height (PH) data channels in HXS and GRS are re-calibrated by using the data of the whole mission period. Secular
gain changes are recognized in HXS, and the characteristics of power-law flare spectra simultaneously observed by HXT and
HXS confirms the trend. The GRS gains are different for the flare observations during the previous maximum and for the current
maximum. The total of 33 γ -ray events are observed, and for 12 of them γ-ray flare spectra are obtained.
Electronic supplementary material to this article is available at and is accessible for authorized users. |
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