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https://www.ias.ac.in/article/fulltext/joaa/036/01/0233-0254

MHD waves—Kelvin–Helmholtz instability—coronal mass ejections.

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.

I. Zhelyazkov¹

1. Faculty of Physics, Sofia University, BG-1164 Sofia, Bulgaria.

Published

March 2015

Manuscript received

11 December 2014

Accepted

20 February 2015