How Rotating Solar Atmospheric Jets Become Kelvin--Helmholtz Unstable.

摘要: Recent observations support the propagation of a number magnetohydrodynamic (MHD) modes which, under some conditions, can become unstable and developing instability is Kelvin--Helmholtz (KHI). In its nonlinear stage KHI trigger occurrence wave turbulence which considered as candidate mechanism for coronal heating. We review modeling tornado-like phenomena in solar chromosphere corona moving weakly twisted spinning cylindrical flux tubes, showing that rises at excitation high-mode MHD waves. The occurs within wavenumber range whose width depends on mode \emph{m}, plasma density contrast between rotating jet environment, also twists internal magnetic field velocity. have studied two polar hole jets, emerging from filament eruption, macrospicule. theoretically calculated development times few minutes wavelengths comparable to half-widths jets are good agreement with observationally determined growth only high order (10 $\mathrm{\leqslant}$ \emph{m} 65) modes. Therefore, we expect observed these cases due high-order