On the nature of kink MHD waves in magnetic flux tubes
By M. Goossens, J. Terradas, Jesse Andries, I. Arregui, J. Ballester. 2009
193 citations recorded by the source corpus.
Context. Magnetohydrodynamic (MHD) waves are often reported in the solar atmosphere and usually classified as slow, fast, or Alfven. The possibility that these waves have mixed properties is often ignored. Aims. The goal of this work is to study and determine the nature of MHD kink waves. Methods. This is done by calculating the frequency, the damping rate and the eigenfunctions of MHD kink waves for three widely different MHD waves cases: a compressible pressure-less plasma, an incompressible plasma and a compressible plasma which allows for MHD radiation. Results. In all three cases the frequency and the damping rate are for practical purposes the same as they differ at most by terms proportional to (kzR) 2 . In the magnetic flux tube the kink waves are in all three cases, to a high degree of accuracy incompressible waves with negligible pressure perturbations and with mainly horizontal motions. The main restoring force of kink waves in the magnetised flux tube is the magnetic tension force. The total pressure gradient force cannot be neglected except when the frequency of the kink wave is equal or slightly differs from the local Alfven frequency, i.e. in the resonant layer. Conclusions. Kink waves are very robust and do not care about the details of the MHD wave environment. The adjective fast is not the correct adjective to characterise kink waves. If an adjective is to be used it should be Alfvenic. However, it is better to realize that kink waves have mixed properties and cannot be put in one single box.
Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics
View Paper: https://www.semanticscholar.org/paper/1141a1fe65fb4c3defa2d76050e34ab0452e0132
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Citations in the corpus
- Multiwavelength Studies of MHD Waves in the Solar Chromosphere (2015, background): “…motions (in the long wavelength limit, i.e., λ a, where λ is the wavelength and a is the radius of the waveguide) and the torsional Alfvén mode (for theoretical discussions of the individual mode properties see, e.g., Spruit 1982; Edwin and Roberts 1983; Bennett et al. 1999; Goossens et al. 2009).”
- Alfvén Waves in the Solar Atmosphere (2012, background): “There have been some suggestions that transversal waves may be considered Alfvénic in nature providing that they are incompressible, exhibit no intensity fluctuations and display periodic displacements with the magnetic tension as the restoring force (Goossens et al. 2009).”