On Modeling the Kelvin--Helmholtz Instability in Solar Atmosphere
arXiv:1411.6472 · doi:10.1007/s12036-015-9332-2
Abstract
In the present review article, we discuss the recent developments in studying the Kelvin--Helmholtz (KH) instability of magnetohydrodynamic (MHD) waves propagating in various solar magnetic structures. The main description is on the modeling of KH instability developing in the coronal mass ejections (CMEs), and contributes to the triggering of wave turbulence subsequently leading to the coronal heating. KH instability of MHD waves in coronal active regions recently observed and imaged in unprecedented detail in EUV high cadence, high-resolution observations by SDO/AIA, and spectroscopic observations by Hinode/EIS instrument, is posing now challenge for its realistic modeling. It is shown that considering the solar mass flows of CMEs as moving cylindrical twisted magnetic flux tubes, the observed instability can be explained in terms of unstable m = -3 MHD mode. We also describe the occurrence of the KH instability in solar jets. The obtained critical jet speeds for the instability onset as well as the linear wave growth rates are in good agreement with the observational data of solar jets.
27 pages, 5 figures, 2 figures added, new references added, accepted. arXiv admin note: text overlap with arXiv:1310.8106, arXiv:1301.2736 by other authors
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Cited by in corpus (5)
- An Analytical Model of the Kelvin-Helmholtz Instability of Transverse Coronal Loop Oscillations
- Kelvin--Helmholtz instability in a twisting solar polar coronal hole jet observed by \emph{SDO}/AIA
- Small-scale solar jet formation and their associated waves and instabilities
- An unstable mode of the stratified atmosphere under the non-traditional Coriolis acceleration
- How Rotating Solar Atmospheric Jets Become Kelvin--Helmholtz Unstable