Abstract
Coronal heating by nanoflares is presented by using observational, analytical, numerical simulation and statistical results. Numerical simulations show the formation of numerous current sheets if the magnetic field is sheared and bipoles have unequal pole strengths. This fact supports the generation of nanoflares and heating by them. The occurrence frequency of transients such as flares, nano/microflares, on the Sun exhibits a power-law distribution with exponent α varying between 1.4 and 3.3. For nanoflares heating α must be greater than 2. It is likely that the nanoflare heating can be reproduced by dissipating Alfven waves. Only observations from future space missions such as Solar-B, to be launched in 2006, can shed further light on whether Alfven waves or nanoflares, heat the solar corona.
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Narain, U., Pandey, K. Nanoflares and heating of the solar corona. J Astrophys Astron 27, 93–100 (2006). https://doi.org/10.1007/BF02702511
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DOI: https://doi.org/10.1007/BF02702511