Coronal Heating by Kink Waves

Astronomy and Astrophysics – Astrophysics

Scientific paper

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7500 Solar Physics, Astrophysics, And Astronomy, 7509 Corona, 7524 Magnetic Fields

Scientific paper

We examine the hypothesis that kink waves contribute to coronal heating. In earlier work we demonstrated that the excitation of kink oscillations flux tubes in the magnetic network of the Sun through their footpoint motions can provide sufficient energy for chromospheric heating. This calculation assumed that: (a) the waves could be treated using the linear approximation, and (b) the kink and longitudinal waves were decoupled. These approximations, although valid in the lower atmosphere, break down in the upper chromosphere, where the wave amplitude becomes comparable with the tube speed. We overcome the earlier limitations by numerically solving the nonlinear MHD equations for coupled kink and longitudinal waves. Using a specified form of the footpoint motions, which is compatible with observations, we solve the nonlinear time-dependent MHD equations for a thin flux tube extending vertically from the sub-photosphere to the base of the corona. Our code is able to resolve shocks and also self-consistently treats mode transformation. We calculate the energy fluxes in vertically propagating kink waves and show that there is in principle adequate energy in the waves to heat the corona.

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