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High Energy Phenomena in the Sun

Published online by Cambridge University Press:  14 August 2015

Claudio Chiuderi*
Affiliation:
Istituto di Astronomia, Università di Firenze, Italy

Extract

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High energy phenomena in the solar physics context, simply means solar flares. To be sure, the energies attained during flares are certainly not very impressive on a cosmic-ray scale. The most energetic particles belong the GeV range, the highest temperatures are of the order of 107 K, γ-ray emission is occasional and the total energy emitted remains below 1033 ergs for all the flares so far observed. Apart from an absolute energy scale, flares are also energetically irrelevant on a solar scale. In fact in a large flare a few units in 1032 ergs are emitted, with a total duration of about one hour and a total surface area involved of a few units in 10−4 of the solar surface. Recalling the values of the luminosity, L ≃ 4 × 1033 erg s−1 and the solar flux F6.3 × 1010 erg cm−2s−1, we see that

Type
Research Article
Copyright
Copyright © Reidel 1981 

References

The literature on solar flares is very vast. We list here a few recent review papers or books to which we refer for an extensive bibliography Google Scholar
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Rust, D.M. 1980, Solar System Plasma Physics, (Kennel, C.F., Lanzerotti, L.J. and Parker, E.N., Eds.), North-Holland, New York, USA.Google Scholar
Sakurai, K.: 1974, Astrophys. Space Sci. 28, 375.CrossRefGoogle Scholar
Sturrock, P.A. (Ed.): 1980, Solar Flares, Proceedings of the Second Skylab Workshop, Univ. of Colorado Press, Boulder, USA.Google Scholar
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