Masuda flare: Difference between revisions
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imported>Schriste (New page: Occurred on 13 January 1992. Intriguing due to Masuda (1994) discovery of a HXR source above the loop top up to > 100 keV. The existence of the Masuda source is still not well understood...) |
imported>Hhudson No edit summary |
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A flare event (SOL1992-01-13, M2.0) observed by Yohkoh at the E limb of the Sun ([http://adsabs.harvard.edu/abs/1994Natur.371..495M Ref. 1]). | |||
As of 2014 there had been more than 500 citations of this very influential paper. | |||
The appearance of a hard X-ray source source distinctly ''above'' the tops of ordinary-looking flare loops, and observable up to above 100 keV, convinced many people of the correctness of | |||
standard ideas of magnetic reconnection as an explanation for how flares work. | |||
Decisive observations have been elusive, unfortunately, possibly because such flares are extremely rare. | |||
== References == | == References == | ||
[1] [http://adsabs.harvard.edu/abs/1994Natur.371..495M "A loop-top hard X-ray source in a compact solar flare as evidence for magnetic reconnection"] | |||
Latest revision as of 14:55, 5 January 2015
A flare event (SOL1992-01-13, M2.0) observed by Yohkoh at the E limb of the Sun (Ref. 1). As of 2014 there had been more than 500 citations of this very influential paper. The appearance of a hard X-ray source source distinctly above the tops of ordinary-looking flare loops, and observable up to above 100 keV, convinced many people of the correctness of standard ideas of magnetic reconnection as an explanation for how flares work. Decisive observations have been elusive, unfortunately, possibly because such flares are extremely rare.
References
[1] "A loop-top hard X-ray source in a compact solar flare as evidence for magnetic reconnection"