Chromospheric evaporation in a well-observed compact flare

Details Chromospheric evaporation in a well-observed compact flare Chromospheric evaporation in a well-observed compact flare

Dec 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982apj...263..409a&link_type=abstract

Astrophysical Journal, Part 1, vol. 263, Dec. 1, 1982, p. 409-422. Research supported by the Lockheed Independent Research Prog

Other

78

Chromosphere, Solar Atmosphere, Solar Flares, Solar X-Rays, Evaporation, H Alpha Line, Solar Maximum Mission, X Ray Spectra

Scientific paper

Hudson and Ohki (1972) pointed out that the increase of the soft X-ray emission measure during flares might be accounted for in two different ways, either by 'coronal condensation', or by what they termed 'chromospheric rarefaction', now more commonly called 'chromospheric evaporation'. They ruled out coronal condensation on the basis of cornal mass content arguments. Moore et al. (1980) found it highly probable that the bulk of the mass of the soft X-ray emitting plasma is supplied during the rise phase by chromospheric evaporation from the feet of the soft X-ray loops. On the other hand, Cheng et al. (1981) argued that chromospheric evaporation is not important as a source of soft X-ray plasma. The present investigation is concerned with an event in which direct chromospheric observations contradict the conclusions reached by Cheng et al. Up to now chromospheric evaporation has always been an inference, without compelling positive evidence. In the current investigation, observations are considered which constitute such evidence.

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