EDP Sciences
Free Access
Volume 408, Number 2, September III 2003
Page(s) 755 - 765
Section Diffuse matter in space
DOI https://doi.org/10.1051/0004-6361:20030984
Published online 17 November 2003

A&A 408, 755-765 (2003)
DOI: 10.1051/0004-6361:20030984

The damping of slow MHD waves in solar coronal magnetic fields

I. De Moortel and A. W. Hood

School of Mathematics and Statistics, University of St Andrews, North Haugh, St Andrews, Fife KY16 9SS, Scotland
(Received 18 April 2003 / Accepted 17 June 2003)

A theoretical description of slow MHD wave propagation in the solar corona is presented. Two different damping mechanisms, namely thermal conduction and compressive viscosity, are included and discussed in detail. We revise the properties of the "thermal" mode, which is excited when thermal conduction is included. The thermal mode is purely decaying in the case of standing waves, but is oscillatory and decaying in the case of driven waves. When thermal conduction is dominant, the waves propagate largely undamped, at the slower, isothermal sound speed. This implies that there is a minimum damping time (or length) that can be obtained by thermal conduction alone. The results of numerical simulations are compared with TRACE observations of propagating waves, driven by boundary motions, and standing waves observed by SUMER/SOHO, excited by an initial impulse. For typical coronal conditions, thermal conduction appears to be the dominant damping mechanism.

Key words: Sun: corona -- Sun: activity -- magnetohydrodynamics (MHD)

Offprint request: I. De Moortel, ineke@mcs.st-and.ac.uk

© ESO 2003

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