Astronomy and Astrophysics – Astronomy
Scientific paper
Jul 1983
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983ssrv...35..259s&link_type=abstract
Space Science Reviews (ISSN 0038-6308), vol. 35, July 1983, p. 259-267. Research supported by the Koninklijkc Nederlandse Akadem
Astronomy and Astrophysics
Astronomy
8
Chromosphere, Coronal Loops, Noise Storms, Solar Flares, Solar Maximum Mission, Solar Radio Bursts, Astronomical Models, Brightness Distribution, Solar Storms, Spaceborne Astronomy
Scientific paper
The gigantic arches in the corona detected by the Hard X-ray Imaging Spectrometer aboard the SMM are stationary, and they form the base of a stationary type I radio noise storm initiated by the flare. They are visible in X rays for ten hours and more and may be revived, in temperature, density, and brightness, if another two-ribbon flare appears below them. It is suggested that they are built up through a reconnection process during the flare from the upper reconnected loops in the Kopp and Pneuman (1976) model. Striking brightness variations are seen quasi-periodically in the corona below and above the arch a few hours after the flare. The variations are seen at about the same time in soft X rays, hard X rays, and on centimeter microwaves in the low corona, as well as at metric waves in the type I noise-storm region. Despite their flarelike intensity, however, the variations have little response in the transition layer (O V line) and no response at all in the chromosphere (H-alpha). It is suggested that these semiperiodic brightenings derived from repetitive acceleration processes in plasmoids that encircle the arch perpendicular to the H-parallel = 0 line from the low corona through the noise storm region, being completely detached from the lower atmospheric layers.
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