Speaker
Description
We theoretically investigate the interplay between magnetohydrodynamic (MHD) waves and shear flows in a partially ionized solar plasma, focusing on the energy exchange mediated by the flow and the transformation between wave modes. We consider a simple model composed of a uniform partially ionized plasma with a straight magnetic field. A shear flow is present in the direction of the magnetic field with a velocity that varies linearly across the magnetic field. The linearized MHD equations in the single-fluid approximation are used, which include the ambipolar diffusion term due to ion-neutral collisions. A nonmodal approach is adopted, in order to convert the flow spatial inhomogeneity into a temporal one, adding a temporal dependence into the component of the wavevector in the direction of the flow inhomogeneity. A system of three ordinary differential equations is derived, which generally governs the temporal evolution of the coupled MHD waves, their interaction with the shear flow, and their ambipolar damping. Numerical solutions are computed to study the coupling and mutual transformation between the fast magnetosonic wave and the Alfvén wave. A detailed parameter study is conducted, demonstrating how the energy transfer and mode transformation are affected. The role of ambipolar diffusion is investigated by comparing the results of the ideal case with those obtained when ambipolar diffusion is included. It is found that ambipolar diffusion can significantly affect the efficiency of the energy exchange between modes and introduces a new coupling mechanism. Additionally, a specific application to solar prominence threads is included, showing that wave coupling and energy exchange can occur within these and other similar structures in the solar atmosphere.
| Sessions | Wave generation, energy transport, dissipation and heating |
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