Astronomy and Astrophysics – Astrophysics
Scientific paper
Jun 1994
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994a%26a...286..952m&link_type=abstract
Astronomy and Astrophysics 286, 952-961 (1994)
Astronomy and Astrophysics
Astrophysics
9
Sun: Corona, Sun: Oscillations, Mhd, Methods: Numerical
Scientific paper
Numerical simulations are performed to investigate the excitation of magnetohydrodynamic waves in coronal loops by photospheric shearing motions. In the simulations the solar coronal loop is modelled as a straight slab of enhanced gas density. The plasma is described by magnetohydrodynamic equations that include finite gas pressure effects and magnetic diffusivity. The Alfven wave is artificially suppressed from the system. MHD waves are excited by imposing oscillations at one end of the plasma slab. A plasma responds to a foot-point motion by kink or sausage waves in dependence on the polarization of a driver. The foot-point motion induces a growth in the parallel velocity. The growth occurs in a resonant layer on a time scale which is much less than a typical life time of a loop. The heating associated with the resonant absorption of the waves is very small and can thus not be considered as relevant for the coronal heating mechanism. The nonlinearity of the MHD equations gives rise to a distorted plasma flow, introducing an asymmetry in the system, and speeds up the occurrence of the resonant layer.
Goossens Marcel
Murawski Kris
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