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Nonlin. Processes Geophys., 14, 649-654, 2007
https://doi.org/10.5194/npg-14-649-2007
© Author(s) 2007. This work is licensed under
the Creative Commons Attribution-NonCommercial-ShareAlike 2.5 License.
 
24 Oct 2007
Intermittent heating of the solar corona by MHD turbulence
É. Buchlin Space and Atmospheric Physics group, Blackett Laboratory, Imperial College, London, UK
Abstract. As the dissipation mechanisms considered for the heating of the solar corona would be sufficiently efficient only in the presence of small scales, turbulence is thought to be a key player in the coronal heating processes: it allows indeed to transfer energy from the large scales to these small scales. While Direct numerical simulations which have been performed to investigate the properties of magnetohydrodynamic turbulence in the corona have provided interesting results, they are limited to small Reynolds numbers. We present here a model of coronal loop turbulence involving shell-models and Alfvén waves propagation, allowing the much faster computation of spectra and turbulence statistics at higher Reynolds numbers. We also present first results of the forward-modelling of spectroscopic observables in the UV.

Citation: Buchlin, É.: Intermittent heating of the solar corona by MHD turbulence, Nonlin. Processes Geophys., 14, 649-654, https://doi.org/10.5194/npg-14-649-2007, 2007.
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