Physics
Scientific paper
May 1976
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1976rspta.281..443b&link_type=abstract
(Royal Society, Discussion on the Physics of the Solar Atmosphere, London, England, Jan. 14, 15, 1975.) Royal Society (London),
Physics
36
Far Ultraviolet Radiation, Solar Flares, Solar Radiation, Ultraviolet Spectroscopy, Electron Density (Concentration), Emission Spectra, Fine Structure, Forbidden Bands, Ion Temperature, Red Shift, Solar X-Rays, Spectrum Analysis, Ultraviolet Photometry, Ultraviolet Spectrometers
Scientific paper
The paper summarizes observations of selected solar flares made with a far-UV spectroheliograph (190-465 A) and a UV spectrograph (900-1900 A) aboard Skylab. The emission lines used in the present analysis are identified, and three events are described in detail: the flare of June 15, 1973, a small subflare observed on August 9, 1973, and the flare of January 21, 1974. Ultraviolet images of two other events are also presented in an attempt to sketch a general picture of a flare as seen in this spectral region. It is found that a small kernel seems to be the source of the primary energy release of a flare. The size, electron density, and ion temperature of a typical kernel are estimated, and it is noted that hot clouds of coronal gas at 20 million K surrounded the observed kernels. It is speculated that flare kernels might be very thin channels through which high-energy particles, originating in deep layers, are ejected into the corona.
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