Solar flare observations and their interpretations

Details Solar flare observations and their interpretations Solar flare observations and their interpretations

Jul 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981nassp.450..181b&link_type=abstract

In NASA. Goddard Space Flight Center The Sun as a Star p 181-227 (SEE N81-27008 17-90)

Physics

8

Magnetic Disturbances, Solar Flares, Solar X-Rays, Electromagnetic Radiation, Sun, Sunspots

Scientific paper

A solar flare has a characteristic spatial extent of 10,000 to 100,000 km. It develops rapidly, with a characteristic time scale of 100 to 1000 s but its manifestations can be observed for hours after onset. A solar flare is the source of highly energetic particles with energies that extend into the GeV range; it produces copious amounts of electromagnetic radiation from gamma-rays to wavelengths of 10 km; and it produces violent magnetohydrodynamic phenomena such as shocks and fast mass ejections. The three basic phases of a flare are described and are: the precursor (preflare) phase, lasting for minutes to hours; the flash phase, lasting for 1 to 5 minutes; and the main (gradual) phase, lasting, on occasion, for hours.

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