Abstract
A brief review is given of the initial six months (October 1991 – March 1992) of solar flare observations with the Hard X-ray Telescope (HXT) aboard Yohkoh. The Yohkoh HXT has the following advanced capabilities: (i) four-band, simultaneous imaging in the X-ray energy ranges of 14–23, 23–33, 33–53, and 53–93 keV; (ii) high angular resolution of ∼ 5 arcsec with a wide Held of view covering the whole Sun; (iii) high time resolution of 0.5 s; and (iv) high sensitivity with a total effective area exceeding 50 cm2. More than 250 solar flares were observed in the initial six months, including four GOES X-class flares. It was revealed that hard X-ray sources of flares are much more complicated than expected; they sometimes vary quite rapidly, and even at the same time they show different shapes at different X-ray energies. Typical features were derived, however, from observations of several well-analyzed flares. Their implications for the particle acceleration mechanisms of solar flares are discussed.
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© 1993 Kluwer Academic Publishers
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Kosugi, T. (1993). Hard X-Ray Solar Flares Observed by Yohkoh and Particle Acceleration. In: Linsky, J.F., Serio, S. (eds) Physics of Solar and Stellar Coronae: G.S. Vaiana Memorial Symposium. Astrophysics and Space Science Library, vol 183. Springer, Dordrecht. https://doi.org/10.1007/978-94-011-1964-1_10
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DOI: https://doi.org/10.1007/978-94-011-1964-1_10
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