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Chromospheric evaporation in a well-observed compact flare

1982; IOP Publishing; Volume: 263; Linguagem: Inglês

10.1086/160513

1538-4357

L. W. Acton, J. W. Leibacher, R. C. Canfield, T. A. Gunkler, H. S. Hudson, A. L. Kiplinger,

Ionosphere and magnetosphere dynamics

view Abstract Citations (110) References (43) Co-Reads Similar Papers Volume Content Graphics Metrics Export Citation NASA/ADS Chromospheric evaporation in a well-observed compact flare Acton, L. W. ; Leibacher, J. W. ; Canfield, R. C. ; Gunkler, T. A. ; Hudson, H. S. ; Kiplinger, A. L. Abstract 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. Publication: The Astrophysical Journal Pub Date: December 1982 DOI: 10.1086/160513 Bibcode: 1982ApJ...263..409A Keywords: Chromosphere; Solar Atmosphere; Solar Flares; Solar X-Rays; Evaporation; H Alpha Line; Solar Maximum Mission; X Ray Spectra; Solar Physics full text sources ADS |