Book contents
- Frontmatter
- Dedication
- Contents
- Preface
- 1 General Principles
- 2 Waves in a Uniform Medium
- 3 Magnetically Structured Atmospheres
- 4 Surface Waves
- 5 Magnetic Slabs
- 6 Magnetic Flux Tubes
- 7 The Twisted Magnetic Flux Tube
- 8 Connection Formulas
- 9 Gravitational Effects
- 10 Thin Flux Tubes: The Sausage Mode
- 11 Thin Flux Tubes: The Kink Mode
- 12 Damping
- 13 Nonlinear Aspects
- 14 Solar Applications of MHD Wave Theory
- References
- Index
12 - Damping
Published online by Cambridge University Press: 15 July 2019
- Frontmatter
- Dedication
- Contents
- Preface
- 1 General Principles
- 2 Waves in a Uniform Medium
- 3 Magnetically Structured Atmospheres
- 4 Surface Waves
- 5 Magnetic Slabs
- 6 Magnetic Flux Tubes
- 7 The Twisted Magnetic Flux Tube
- 8 Connection Formulas
- 9 Gravitational Effects
- 10 Thin Flux Tubes: The Sausage Mode
- 11 Thin Flux Tubes: The Kink Mode
- 12 Damping
- 13 Nonlinear Aspects
- 14 Solar Applications of MHD Wave Theory
- References
- Index
Summary
The effect of damping by magnetic diffusivity and viscosity is examined for an Alfven wave in a non-uniform atmosphere, demonstrating the rapidity of damping when phase mixing operates. A cubic law of damping tends to apply, though this may apply only after a transition stage or time. Damping when phase mixing is absent and when it is operative is illustrated for coronal conditions. The various approximations used in the derivation of such results are examined. Damping by a slow wave under the influence of viscosity and thermal conductivity is explored at length. Results are illustrated for coronal conditions. Both temporal and spatial behaviours are investigated.
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- MHD Waves in the Solar Atmosphere , pp. 360 - 396Publisher: Cambridge University PressPrint publication year: 2019