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Paper: Propagation and Dissipation of Slow Magnetosonic Waves in Coronal Plumes
Volume: 205, The Last Total Solar Eclipse of the Millennium in Turkey
Page: 147
Authors: Ofman, L.
Abstract: Recently, slow magnetosonic waves were identified in polar plumes at heights of up to ~1.2Rodot using the Extreme Ultraviolet Imaging Telescope (EIT) on board the Solar and Heliospheric Observatory (SOHO) spacecraft. We model the propagation of these waves in solar polar coronal plumes, and the dissipation of the waves by compressive viscosity. First, we estimate the damping rate of the waves using linear theory. Next, we model the slow magnetosonic wave with a 2D MHD code in spherical geometry and assume azimuthal symmetry of the plumes. We find that the slow magnetosonic waves generated at the base of the plumes by periodic compressions propagate outward and dissipate in the plumes. The background atmosphere includes Parker's flow and the corresponding density stratified by gravity close to the Sun. The stratification leads to the nonlinear steepening, and to enhanced dissipation over the linear rate of the waves. The dissipation may contribute to the heating and the acceleration of the solar wind. By observing the density structure of the plumes during an eclipse it may be possible to learn more about these waves.
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