The continuous spectrum of MHD waves in 2-D solar loops and arcades - Parametric study of poloidal mode coupling for poloidal magnetic fields

Details The continuous spectrum of MHD waves in 2-D solar loops and arcades - Parametric study of poloidal mode coupling for poloidal magnetic fields The continuous spectrum of MHD waves in 2-D solar loops and arcades - Parametric study of poloidal mode coupling for poloidal magnetic fields

Jun 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988a%26a...198..331p&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 198, no. 1-2, June 1988, p. 331-340.

Physics

13

Coronal Loops, Magnetohydrodynamic Waves, Plasma Heating, Plasmas (Physics), Poloidal Flux, Solar Corona, Cartesian Coordinates, Chromosphere, High Temperature Plasmas, Photosphere, Wave Functions

Scientific paper

This parametric study investigates how poloidal mode coupling of ideal MHD continuum modes of two-dimensional models for coronal loops and arcades depends on equilibrium quantities. The two physical causes for poloidal mode coupling considered are non-circularity of the cross-sections of the flux surfaces and variation of the equilibrium density along the magnetic field lines. This phenomenon of wave number coupling is typical for the continuous spectrum of MHD waves of 2D plasmas. It has two important consequences: the eigenfrequencies are modified, and the eigenfunctions tend to localize. The present parametric study is concerned with the dependence of poloidal mode coupling on the value of the plasma beta (i.e. the ratio of the plasma pressure to the magnetic pressure), the ellipticity of the cross-sections, and the variation of the equilibrium density normal to the magnetic surfaces and along the magnetic field lines. For realistic values of the parameters, it is found that the continuous spectrum is modified, the ranges of the continuum frequencies are considerably enlarged, and the derivatives of the continuum frequencies normal to the magnetic surfaces are considerably increased. Consequently, the phasemixing time is reduced, and the efficiency of phase-mixing as a heating mechanism of solar loops and arcades is increased. The dissipation of wave energy depends on two spatial coordinates and is found to be larger at the tops of the coronal loops.

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