Very impulsive solar flares observed with the YOHKOH spacecraft

Details Very impulsive solar flares observed with the YOHKOH spacecraft Very impulsive solar flares observed with the YOHKOH spacecraft

Feb 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...421..843f&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 421, no. 2, p. 843-850

Astronomy and Astrophysics

Astronomy

49

Electron Energy, Gamma Ray Astronomy, Gamma Ray Spectra, Solar Flares, Solar Spectra, Spaceborne Astronomy, X Ray Astronomy, X Ray Spectra, Astronomical Spectroscopy, Japanese Spacecraft, Solar Electrons, Solar Wind, Solar X-Rays, Spectrometers, X Ray Spectroscopy, X Ray Telescopes

Scientific paper

Using X-ray data from two instruments aboard the Yohkho spacecraft, launched in 1991 August to study solar high-energy phenomena, some 38 extremely impulsive flares of X-ray importance greater than C1 have been identified and studied. Electron temperatures of these flares, derived from Yohkoh Bent Crystal Spectrometer data, appear to decline immediately after the intensity maximum is attained, implying that energy input into the flaring plasma is reduced or possibly ceases after this time. Images of these flares with the high-resolution Yohkoh Soft X-ray Telescope show that, contrary to expectation if thermal conduction is a significant cooling mechanism, the emitting regions of tiny pointlike sources (volumes less than or = 3 x 1024cc) within a loop structure. With mass loss along field lines eliminated also, from a previous study, the chief energy-loss mechanism is likely to be radiation, and if so a lower limit for the electron density of approximately 1012/cc is imposed. This is only compatible with values of the emission measure if the flare volume is 3 x 1024cc, corresponding to a sphere of only 1790 km in diameter.

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