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On Modeling the Kelvin–Helmholtz Instability in Solar Atmosphere

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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 new 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.

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Acknowledgements

This work was supported by the Bulgarian Science Fund and the Department of Science & Technology, Government of India Fund under Indo-Bulgarian bilateral project CSTC/INDIA 01/7, /Int/ Bulgaria/P-2/12. The author is indebted to the referee for his constructive criticism and valuable suggestions for clarifying the paper presentation, Teimuraz Zaqarashvili, Abhishek Srivastava, and Ramesh Chandra for fruitful discussions, and Snezhana Yordanova for drawing one figure.

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Zhelyazkov, I. On Modeling the Kelvin–Helmholtz Instability in Solar Atmosphere. J Astrophys Astron 36, 233–254 (2015). https://doi.org/10.1007/s12036-015-9332-2

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