The development and cooling of a solar limb-flare

Details The development and cooling of a solar limb-flare The development and cooling of a solar limb-flare

Sep 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984mnras.210..443v&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 210, Sept. 15, 1984, p. 443-462. Research supported by

Astronomy and Astrophysics

Astronomy

7

Coronal Loops, Plasma Cooling, Solar Flares, Solar Limb, Solar Magnetic Field, Solar X-Rays, Electron Density (Concentration), H Alpha Line, Magnetic Flux, Solar Maximum Mission, Solar Spectra, Solar Temperature

Scientific paper

Observations of a flare that began in soft X-rays at 20:37 UT on 1980 April 12, at the west limb of the Sun are discussed. The Solar Maximum Mission (SMM) satellite was used to obtain X-ray images before the flare and for a period during the decay phase. Hα photographs and the soft X-ray flux measured by the GOES-3 satellite are available throughout the flare. Some alternative models are discussed but insufficient data are available for a full treatment. Overall, the observations are best fitted qualitatively by a model where pre-existing magnetic loop structures are perturbed by the intrusion of new magnetic flux.

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