Dissipation and Steepening of Slow Magnetosonic Waves in Polar Plumes and the Effect on the Solar Wind Close to the Sun

Details Dissipation and Steepening of Slow Magnetosonic Waves in Polar Plumes and the Effect on the Solar Wind Close to the Sun Dissipation and Steepening of Slow Magnetosonic Waves in Polar Plumes and the Effect on the Solar Wind Close to the Sun

Oct 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999esasp.446..515o&link_type=abstract

8th SOHO Workshop: Plasma Dynamics and Diagnostics in the Solar Transition Region and Corona. Proceedings of the Conference hel

Astronomy and Astrophysics

Astrophysics

Scientific paper

Recently, slow magnetosonic waves were identified in polar plumes at heights up to about 1.2Rs, using Extreme ultraviolet Imaging Telescope (EIT) observations of quasi-periodic EUV intensity fluctuations (Ofman, Nakariakov, DeForest 1999). We model the propagation and dissipation of slow magnetosonic waves in polar plumes using 2D MHD code in spherical geometry. We find that outward propagating slow magnetosonic waves may become trapped due to transverse density and temperature structure of the plumes. The slow waves nonlinearly steepen in the gravitationally stratified plumes. The nonlinear steepening of the waves leads to enhanced acceleration of the subsonic solar wind due to momentum transfer, and to the enhances dissipation due to compressive viscosity at the wave-fronts. The slow waves can contribute to the heating of coronal holes close to the Sun (r<2Rs), a region where the shear Alfven wave heating is inefficient.

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