Abstract
In this article I have discussed the recent ap- proaches in studying the Kelvin-Helmholtz (KH) instability of magnetohydrodynamic (MHD) waves propagating in solar atmo- sphere jets. The main focus is on the modeling the KH instability developing in coronal mass ejections in view of its (instability) contribution to triggering a wave turbulence subsequently leading to an effective coronal heating. KH instability of MHD waves in coronal active regions recently observed and imaged in unprece- dented detail in EUV thanks to the high cadence, high-resolution observations by SDO/AIA instrument, and spectroscopic obser- vations by Hinode/EIS instrument is a challenge for modeling this event. It is shown that considering the solar mass flows of coronal mass ejections as moving cylindrical twisted magnetic flux tubes the imaged instability can be explained in terms of unstable m = 3 MHD mode. Obtained critical jet speeds for the instability onset as well as the linear wave growth rates are in good agreement with observational data.
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