The bright knots at the tops of soft X-ray flare loops: Quantitative results from YOHKOH

Details The bright knots at the tops of soft X-ray flare loops: Quantitative results from YOHKOH The bright knots at the tops of soft X-ray flare loops: Quantitative results from YOHKOH

Feb 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995apj...440..370d&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 440, no. 1, p. 370-385

Astronomy and Astrophysics

Astronomy

47

Coronal Loops, Magnetohydrodynamics, Solar Flares, Solar Magnetic Field, Solar X-Rays, Spaceborne Astronomy, X Ray Astronomy, Astronomical Spectroscopy, Gamma Rays, Japanese Spacecraft, X Ray Telescopes

Scientific paper

Soft X-ray Telescope (SXT) observations from the Japanese Yohkoh spacecraft have shown that confined bright regions are common features at the tops of flare loops throughout most of the duration of the flares. In this paper we present quantitative results for these flare knots, in relation to other flare regions, for four relatively 'simple' flares. Emission measure distributions, electron temperatures, and electron densities are derived from SXT and Yohkoh Bragg Crystal Spectrometer (BCS) observations. The four flares selected are dominated by what appear to be single-loop structures, with bright knots at the loop tops. The flares are neither long-duration nor impulsive events. The spatial distributions of brightness and emission measure in the flares are found to be quite similar for all four events, even though there are significant differences in dynamical behavior between at least two of the events. Temperatures and densities calculated for these flares are consistent with previous results from many solar experiments. An investigation of intensity correlations between adjacent pixels at the tops of the loops suggests the existence of local disturbances in the magnetic loops that occur on spatial scales less than the radii of the loops.

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