| Issue |
A&A
Volume 631, November 2019
|
|
|---|---|---|
| Article Number | A31 | |
| Number of page(s) | 12 | |
| Section | The Sun | |
| DOI | https://doi.org/10.1051/0004-6361/201936198 | |
| Published online | 15 October 2019 | |
Effect of siphon flow on resonant damping of kink oscillations in magnetic flux tubes
1
School of Mathematics and Statistics (SoMaS), The University of Sheffield, Hicks Building, Hounsfield Road, Sheffield S3 7RH, UK
e-mail: m.s.ruderman@sheffield.ac.uk
2
Space Research Institute (IKI) Russian Academy of Sciences, Moscow, Russia
3
National Research University Higher School of Economics, Moscow, Russia
Received:
27
June
2019
Accepted:
5
August
2019
The effect of siphon flow on kink oscillations of magnetic flux tubes is studied in the thin tube and thin boundary layer (TTTB) approximation. The presence of a transitional layer results in oscillation damping due to resonance absorption. To calculate the damping rate we use the regular perturbation method with the ratio of transitional layer thickness to tube radius as a small parameter. We found a dependence of the ratio of decrement to the oscillation frequency, γ/ω1, on the ratio, χ, of flow velocity magnitude to the Alfvén speed in the tube core. The general theoretical results are applied to a particular case where the density radial dependence in the transitional layer is linear. We consider two models. In the first model, the radial dependence of the velocity amplitude is such that the resonance in the transitional layer occurs where the flow velocity is zero. In the second model, the flow velocity is non-zero in the whole transitional layer. In both cases, γ/ω1 is an increasing function of χ. In the first case, the presence of flow can lead to an increase in γ/ω1 by more than a factor of two. In the second model, we only carry out the calculation in the case where the plasma density inside the tube is much larger than the density of the surrounding plasma. In this model, the effect of flow is less pronounced than in the first model, and the presence of flow can increase γ/ω1 by a factor of 0.25 at most. We discuss the application of the obtained results to coronal and prominence seismology. We conclude that while for typical values of velocity in coronal loops the effect of flow is weak, it can be quite substantial in prominence seismology.
Key words: magnetohydrodynamics (MHD) / plasmas / waves / Sun: corona / Sun: magnetic fields / Sun: oscillations
© ESO 2019
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