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Theoretical Foundation of 3D Alfven Resonances
If you have a question about this talk, please contact Robert Teed.
The coupling of fast and Alfven magnetohydrodynamic (MHD) waves is of fundamental interest in astrophysical plasmas. Under certain conditions, Alfven waves can be resonantly excited by fast mode waves, resulting in a localised accumulation of energy in the plasma. In the solar community this is often referred to as resonant absorption, while in the magnetospheric community it’s known as field line resonance. These processes have applications in coronal heating and in magnetospheric dynamics.
Alfven resonances are well understood in 1D and 2D, but not so in 3D. We present a theoretical way of understanding the structure of Alfven resonances in 3D, which is corroborated by numerical simulations.
This talk is part of the DAMTP Astrophysics Seminar series.
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