Reduced MHD Turbulence Model of a Coronal Loop

Details Reduced MHD Turbulence Model of a Coronal Loop Reduced MHD Turbulence Model of a Coronal Loop

May 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...210.3701n&link_type=abstract

American Astronomical Society Meeting 210, #37.01; Bulletin of the American Astronomical Society, Vol. 39, p.150

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It has been found that during flares, the solar coronal emission lines are broader than the thermal width; this broadening corresponds to a nonthermal velocity of the order of 100 km/s (Doschek 1983; Antonucci et al. 1984). Some results (Alexander et al. 1998) suggest that the large values of nonthermal velocity could be related to the actual flare trigger rather than to the later energy deposition. Nigro et al. (2004) have constructed a new MHD turbulence model. This model describe the Alfvenic turbulence inside a coronal loop. It shows that the occurrence of high values (of the order of 100 km/s) of fluctuating velocity at large scale can be an efficient trigger of a non-linear cascade leading to a burst of dissipated energy. This suggests that the observed increase in nonthermal velocities may be an indicator of turbulent changes in the plasma that are related to the flare trigger mechanism. In this presentation we describe a resonant storage of fluctuating magnetic and kinetic energy in a coronal loop and their subsequent dissipation. The dissipation is due to the formation of small scales by a turbulence nonlinear cascade. The intermittent behavior of turbulence described by the model gives rise to bursts of dissipation. The statistics of these bursts compare well with those of the hard X-ray (HXR) emission associated with solar flares.

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