Detection of Waves in the Solar Corona: Kink or Alfvén?

By T. Van Doorsselaere, Valery M. Nakariakov, Erwin Verwichte. 2008

225 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Molecular Biology

View Paper: https://www.semanticscholar.org/paper/aa1e26b02abc9490c9cd1defda38ff0456a37e70

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Citations in the corpus

TIME–DISTANCE SEISMOLOGY OF THE SOLAR CORONA WITH CoMP (2009, methodology): “Recent spectroscopic observations with EIS were used to detect a coronal oscillation and to map the electron density variation across a coronal loop (Van Doorsselaere et al. 2008).”
Quasi-periodic Pulsations in Solar and Stellar Flares: An Overview of Recent Results (Invited Review) (2016, background): “It is even necessary to go beyond simple analytical approximations (like Gruszecki, Nakariakov, and Van Doorsselaere, 2012; Dulk and Marsh, 1982) to correctly predict the emission, especially for the optically thick gyrosynchrotron emission (Reznikova, Antolin, and Van Doorsselaere, 2014).”
Standing Slow-Mode Waves in Hot Coronal Loops: Observations, Modeling, and Coronal Seismology (2010, background): “However, Van Doorsselaere et al. (2008b) suggested that these waves are more likely fast kink waves rather than the true (incompressible) Alfvén mode that is torsional in cylindrical plasma structure and hard to resolve by present instruments.”
The FIP and Inverse FIP Effects in Solar and Stellar Coronae (2015, background): “Alfvén waves which generate the ponderomotive force in the chromosphere have been much harder to detect (Van Doorsselaere et al., 2008), though see Erdélyi and Fedun (2007) and Tomczyk et al. (2007).”
Oscillations and Waves in Solar Spicules (2009, background): “However, most importantly let us emphasise once more that torsional Alfvén waves do not lead to the displacement of tube axis (Erdélyi and Fedun (2007); Van Doorsselaere et al. (2008a); Jess et al. (2009)).”
Alfvén Waves in the Solar Atmosphere (2012, background): “Since torsional Alfvén waves will produce a FWHM oscillation that is 180◦ out of phase at opposite boundaries of the waveguide (Van Doorsselaere et al. 2008), the authors investigated the instantaneous Hα profile at opposite edges of the MBP group.”
Decaying and decayless transverse oscillations of a coronal loop (2013, background): “In terms of magnetohydrodynamic (MHD) wave theory kink oscillations are interpreted as kink (m = 1) fast magnetoacoustic modes (e.g. Edwin & Roberts 1983; Van Doorsselaere et al. 2008), which become weakly compressible in the long-wavelength limit (Goossens et al. 2012).”
On the nature of kink MHD waves in magnetic flux tubes (2009, background): “Subsequently Van Doorsselaere et al. (2008)argued strongly against the possible presence of Alfvén waves in the solar corona emphasising that Alfvén waves cannot be but torsional.”
Magnetohydrodynamic Oscillations in the Solar Corona and Earth’s Magnetosphere: Towards Consolidated Understanding (2016, background): “(40) This formula was numerically checked for larger l/a with an eigenvalue code by Van Doorsselaere et al. (2004a), who found deviations limited to 25 % for the damping time for a broad range of l/a.”