Solar flares, microflares, nanoflares, and coronal heating

Details Solar flares, microflares, nanoflares, and coronal heating Solar flares, microflares, nanoflares, and coronal heating

Jun 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991soph..133..357h&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 133, June 1991, p. 357-369.

Physics

262

Chromosphere, Energy Transfer, Solar Corona, Solar Flares, Atmospheric Heating, Magnetic Field Reconnection, Solar Physics, Thermal Energy

Scientific paper

The established following by solar-flare occurrence of a power-law distribution against total flare energy is seen to imply that microflares must exhibit a steeper distribution if they are energetically significant, and that there must be a high-energy cutoff of the observed distribution. The distribution function presently suggested corresponds to only about 0.5 events, at an astonishing energy of more than 10 to the 32nd ergs/year. Such a distinctively 'soft' distribution is identifiable with Parker's (1983, 1988) nanoflares. Because these events must have a different distribution function, they may also have different physics.

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