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Spatial Damping of Propagating Kink Waves Due to Resonant Absorption: Effect of Background Flow View all abstracts by submitter

Roberto Soler   Submitted: 2011-04-12 02:44

Observations show the ubiquitous presence of propagating magnetohydrodynamic (MHD) kink waves in the solar atmosphere. Waves and flows are often observed simultaneously. Due to plasma inhomogeneity in the perpendicular direction to the magnetic field, kink waves are spatially damped by resonant absorption. The presence of flow may affect the wave spatial damping. Here, we investigate the effect of longitudinal background flow on the propagation and spatial damping of resonant kink waves in transversely nonuniform magnetic flux tubes. We combine approximate analytical theory with numerical investigation. The analytical theory uses the thin tube (TT) and thin boundary (TB) approximations to obtain expressions for the wavelength and the damping length. Numerically, we verify the previously obtained analytical expressions by means of the full solution of the resistive MHD eigenvalue problem beyond the TT and TB approximations. We find that the backward and forward propagating waves have different wavelengths and are damped on length scales that are inversely proportional to the frequency as in the static case. However, the factor of proportionality depends on the characteristics of the flow, so that the damping length differs from its static analogue. For slow, sub-Alfvénic flows the backward propagating wave gets damped on a shorter length scale than in the absence of flow, while for the forward propagating wave the damping length is longer. The different properties of the waves depending on their direction of propagation with respect to the background flow may be detected by the observations and may be relevant for seismological applications.

Authors: Roberto Soler, Jaume Terradas, and Marcel Goossens
Projects: None

Publication Status: Accepted for publication in ApJ
Last Modified: 2011-04-12 08:45
Go to main E-Print page  Instrumental oscillations in RHESSI count rates during solar flares  Propagation of Moreton Waves  Edit Entry  Download Preprint  Submitter's Homepage Delete Entry 

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