Volume 633, January 2020
|Number of page(s)||16|
|Published online||24 January 2020|
Coronal energy release by MHD avalanches: Heating mechanisms
School of Mathematics and Statistics, University of St Andrews, St Andrews, Fife KY16 9SS, UK
e-mail: email@example.com; firstname.lastname@example.org
2 Space and Atmospheric Physics, The Blackett Laboratory, Imperial College, London, SW7 2BW, UK
3 Centre for Fusion, Space and Astrophysics, Department of Physics, University of Warwick, Coventry, CV4 7AL, UK
Accepted: 14 December 2019
The plasma heating associated with an avalanche involving three twisted magnetic threads within a coronal loop is investigated using three-dimensional magnetohydrodynamic simulations. The avalanche is triggered by the kink instability of one thread, with the others being engulfed as a consequence. The heating as a function of both time and location along the strands is evaluated. It is shown to be bursty at all times but to have no preferred spatial location. While there appears to be a level of “background” heating, this is shown to be comprised of individual, small heating events. A comparison between viscous and resistive (Ohmic) heating demonstrates that the strongest heating events are largely associated with the Ohmic heating that arises when the current exceeds a critical value. Viscous heating is largely (but not entirely) associated with smaller events. Ohmic heating dominates viscous heating only at the time of the initial kink instability. It is also demonstrated that a variety of viscous models lead to similar heating rates, suggesting that the system adjusts to dissipate the same amount of energy.
Key words: Sun: corona / Sun: magnetic fields / magnetohydrodynamics (MHD) / methods: numerical
© ESO 2020
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