Harmonic perturbations are studied for a plane parallel model for the solar magnetic atmosphere. In the present model, the magnetic field lines are horizontal, the sound speed and the Alfvén speed are constants. It is known that in this model, analytical solutions can be obtained for linearized perturbations. The harmonic perturbations can either propagate as MHD modes modified by the action of gravity orbe unstable due to magnetic buoyancy. Dispersion properties and stability limits of these waves as well as the growthrates of the instability are displayed for various combinations of parameters: directional angles Φ and θ of wave propagation, wave number k and the plasma parameter β. There are three modes propagating in the considered atmosphere: the fast, the slow and the Alfvén mode, all modified by gravity. Only the modified slow MHD mode can become unstable; the modified Alfvén and fast MHD modes are always stable. In the limit of a vanishing magnetic field the modified fast mode becomes an acoustic gravity mode, the modified Alfvén mode becomes a mode oscillating with the Brunt-Väisälä frequency at large k, while the modified slow mode disappears.
|Number of pages||9|
|Journal||Astronomy and Astrophysics|
|Publication status||Published - 1999|
- Magnetohydrodynamics (MHD)
- Stars: atmospheres