Volume 604, August 2017
|Number of page(s)||10|
|Published online||25 August 2017|
Heating by transverse waves in simulated coronal loops⋆
1 Centre for mathematical Plasma Astrophysics, Department of Mathematics, KU Leuven, Celestijnenlaan 200B, 3001 Leuven, Belgium
2 School of Mathematics and Statistics, University of St. Andrews, St. Andrews, Fife KY16 9SS, UK
Received: 10 February 2017
Accepted: 27 May 2017
Context. Recent numerical studies of oscillating flux tubes have established the significance of resonant absorption in the damping of propagating transverse oscillations in coronal loops. The nonlinear nature of the mechanism has been examined alongside the Kelvin-Helmholtz instability, which is expected to manifest in the resonant layers at the edges of the flux tubes. While these two processes have been hypothesized to heat coronal loops through the dissipation of wave energy into smaller scales, the occurring mixing with the hotter surroundings can potentially hide this effect.
Aims. We aim to study the effects of wave heating from driven and standing kink waves in a coronal loop.
Methods. Using the MPI-AMRVAC code, we perform ideal, three dimensional magnetohydrodynamic (MHD) simulations of both (a) footpoint driven and (b) free standing oscillations in a straight coronal flux tube, in the presence of numerical resistivity.
Results. We have observed the development of Kelvin-Helmholtz eddies at the loop boundary layer of all three models considered here, as well as an increase of the volume averaged temperature inside the loop. The main heating mechanism in our setups was Ohmic dissipation, as indicated by the higher values for the temperatures and current densities located near the footpoints. The introduction of a temperature gradient between the inner tube and the surrounding plasma, suggests that the mixing of the two regions, in the case of hotter environment, greatly increases the temperature of the tube at the site of the strongest turbulence, beyond the contribution of the aforementioned wave heating mechanism.
Key words: magnetohydrodynamics (MHD) / Sun: corona / Sun: oscillations
Three movies associated to Fig. 1 are available in electronic form at http://www.aanda.org
© ESO, 2017
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