The 1992 January 5 Flare at 13.3 UT: Observations from YOHKOH

Details The 1992 January 5 Flare at 13.3 UT: Observations from YOHKOH The 1992 January 5 Flare at 13.3 UT: Observations from YOHKOH

Oct 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993apj...416..845d&link_type=abstract

Astrophysical Journal v.416, p.845

Astronomy and Astrophysics

Astronomy

22

Sun: Flares, Sun: Magnetic Fields, Sun: X-Rays, Gamma Rays

Scientific paper

We discuss X-ray spectra and soft X-ray images of an M1.9 flare that occurred on 1992 January 5 near 13.3 UT. These data were obtained with instrumentation on the Japanese Yohkoh spacecraft. They cover the entire rise phase of the flare. To supplement these data we have ground-based magnetograms and Hα spectroheliograms. We calculate the electron temperature and emission measure of the flare as a function of time during the early rise phase using X-ray spectral line intensities and line ratios. Using spectral line widths, line profile asymmetries, and wavelength shifts due to the Doppler effect, we calculate the dynamical properties of the flare. The time development of the morphology of the flare, as revealed by the soft X-ray images and the Hα spectroheliograms, and the physical quantities inferred from the X-ray spectra, are compared with chromospheric evaporation models. There is an enhancement of blueshifted emission that is closely correlated with the hard X-ray bursts. Heating of one loop in the flare is consistent with a conduction-evaporation model, but heating is found in several structures that do not appear to be physically associated with each other. No standard evaporation model can adequately explain all of the observations.

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