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Solar Physics

, 294:20 | Cite as

Can High-Mode Magnetohydrodynamic Waves Propagating in a Spinning Macrospicule Be Unstable Due to the Kelvin–Helmholtz Instability?

  • I. ZhelyazkovEmail author
  • R. Chandra
Article

Abstract

We investigate the conditions at which high-mode magnetohydrodynamic (MHD) waves propagating in a spinning solar macrospicule can become unstable with respect to the Kelvin–Helmholtz instability (KHI). We consider the macrospicule as a weakly twisted cylindrical magnetic flux tube moving along and rotating around its axis. Our study is based on the dispersion relation (in complex variables) of MHD waves obtained from the linearized MHD equations of an incompressible plasma for the macrospicule and cool (\(\beta = 0\), with \(\beta\) the plasma to the magnetic pressure) plasma for its environment. This dispersion equation is solved numerically using appropriate input parameters to find out an instability region or window that accommodates suitable unstable wavelengths on the order of the macrospicule width. It is established that an \(m = 52\) MHD mode propagating in a macrospicule with width of 6 Mm, axial velocity of \(75~\mbox{km}\,\mbox{s}^{-1}\), and rotating one of \(40~\mbox{km}\,\mbox{s}^{-1}\) can become unstable against the KHI with growth times of 2.2 and 0.57 min at 3 and 5 Mm unstable wavelengths, respectively. These growth times are much shorter than the macrospicule lifetime, which lasts about 15 min. An increase or decease in the width of the jet would change the KHI growth times, which remain more or less of the same order when they are evaluated at wavelengths equal to the width or radius of the macrospicule. It is worth noting that the excited MHD modes are super-Alfvénic. A change in the background magnetic field can lead to another MHD mode number, \(m\), that ensures the required instability window.

Keywords

Magnetohydrodynamics MHD waves and instability Solar macrospicules 

Notes

Acknowledgements

Our work was supported by the Bulgarian Science Fund under project DNTS/INDIA 01/7. The authors are indebted to the anonymous reviewer for pointing out a mathematical error and for the helpful and constructive comments and suggestions that contributed to improving the final version of the manuscript.

Disclosure of Potential Conflicts of Interest

The authors declare that they have no conflicts of interest.

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Copyright information

© Springer Nature B.V. 2019

Authors and Affiliations

  1. 1.Faculty of PhysicsSofia UniversitySofiaBulgaria
  2. 2.Department of Physics, DSB CampusKumaun UniversityNainitalIndia

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