Kelvin-Helmholtz Instability in Solar Spicules

Magneto hydrodynamic waves, propagating along spicules, may become unstable and the expected instability is of kelvinhelmholtz type. such instability can trigger the onset of wave turbulence leading to an effective plasma heating and particle acceleration. in present study, twodimensional magneto hydrodynamic simulations performed on a cartesian grid is presented in spicules with different densities, moving at various speeds depending on their environment. simulations being applied in this study show the onset of kelvinhelmholtz type instability and transition to turbulent flow in spicules. development of kelvinhelmholtz instability leads to momentum and energy transport, dissipation, and mixing of fluids. when magnetic fields are involved, field amplification is also possible to take place