Volume 437, Number 3, July III 2005
|Page(s)||L47 - L50|
|Published online||30 June 2005|
Letter to the Editor
Damping of phase-mixed slow magneto-acoustic waves: Real or apparent?
Centrum voor Plasma-astrofysica, K. U. Leuven, Celestijnenlaan 200B, 3001 Leuven, Belgium e-mail: firstname.lastname@example.org
Accepted: 29 May 2005
The propagation of slow magnetoacoustic waves along a multithreaded coronal loop is modelled analytically by means of a ray tracing method. It is shown how cross field gradients build up due to phase mixing. The cross field gradients can enhance shear viscosity so that it dominates over compressive viscosity. Nevertheless the short dissipation distances (~107 m) observed for slow waves in coronal loops require very small cross field length scales which imply a filamentary structure on scales at least three orders of magnitude below the current detection limit of TRACE and close to the limit where magnetohydrodynamic (MHD) theory breaks down. The observed dissipation distances can alternatively be explained by phase mixing in its ideal regime, where the apparent damping is due to the spatial integration of the phase mixed amplitudes by the observation.
Key words: Sun: corona / Sun: magnetic fields / Sun: oscillations / plasmas / waves
© ESO, 2005
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