Weak Transient Activities in the Corona

Details Weak Transient Activities in the Corona Weak Transient Activities in the Corona

Dec 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999spro.proc..123s&link_type=abstract

Solar Physics with Radio Observations, Proceedings of the Nobeyama Symposium, held in Kiyosato, Japan, Oct. 27-30, 1998, Edited

Physics

Scientific paper

Weak transient activities of small-scale coronal loops have been reported from Yohkoh and SoHO observations: Active-region transient brightenings (ARTBs), XBP flares, network flares, coronal flashes, and EUV transient brightenings. They are called with different terminology, but no significant differences can be found except for the sizes of energy and the locations where they are observed on the Sun. No differences except for the sizes of energy can be also found between ARTBs and standard flares; The frequency distribution of ARTBs as a function of energy is well represented by a single power-law with a slope similar to that of standard flares, and relatively strong ARTBs are populated by non-thermal electrons. With these observations, although more observations are still required, we currently conclude that weak transient activities of small-scale coronal loops observed not only in active regions but also in quiet regions are just small flares (microflares or nanoflares in terminology), which are located in lower energy extension of standard flares. No reliable evidences suggesting that microflares or nanoflares entirely explain the heating of the corona have been found. However, weak temporal variations seen in quasi-steady long loops are found to be well correlated with the heating level, suggesting that they may be an X-ray signature of the heating process responsible for the heating of the corona.

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