A study of the morphology of solar flares as observed by the hard X-ray imaging spectrometer

Details A study of the morphology of solar flares as observed by the hard X-ray imaging spectrometer A study of the morphology of solar flares as observed by the hard X-ray imaging spectrometer

Nov 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984esasp.220..281h&link_type=abstract

In ESA The Hydromagnetics of the Sun p 281-282 (SEE N85-25091 14-92)

Physics

2

Solar Flares, Solar Maximum Mission, Solar X-Rays, Coronal Loops, Solar Radio Bursts, X Ray Spectroscopy

Scientific paper

The hard X-ray imaging spectrometer on board the Solar Maximum Mission observed several hundred solar flares in the 3.5 to 30 keV energy region. Analysis of a subset of these events, chosen to represent all active regions viewed shows that the majority of flares conform to the scenario; in 3.5 to 30 keV X-rays, the impulsive burst defines a system of low lying coronal magnetic loops. The soft X-ray flare expands into a larger, well resolved loop system and frequently an even larger overlying structure is involved with foot points separated by several hundred thousand km. A flare model involving a single magnetic loop is rarely, if ever, appropriate.

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