Kelvin–Helmholtz instability in non-Maxwellian magnetized dusty plasmas

Kelvin–Helmholtz instability (KHI) is investigated in the context of a non-Maxwellian dusty plasma comprising of electrons, ions and dust particles. The generalized dispersion relation is derived, which is of a complex nature due to some of the source terms like density inhomogeneity and sheared flow A that are responsible for instability in the system. To discuss the instability, the dispersion relation is solved numerically to discuss the growth rates. The primary goal is to understand the dynamics of KH modes in non-Maxwellian plasmas defined by the Kappa and Cairns distribution parameters influence the creation and features of KHI. We have found that the development rates and threshold conditions for these instabilities are significantly altered in the presence of non-Maxwellian distributions, influencing the overall dynamics of space plasma environment. The results demonstrate that superthermal particles in the Cairns distribution speed up the KHI's development rate, but the Kappa parameter has a more stable influence in comparison with Cairns. The effects of different parameters are investigated like sheared velocity, magnetic field, and dust mass. Dust particles present there strongly influence the system dynamics by increasing the chances of growing modes. Increasing dust mass can produce more obvious instabilities in celestial environments such as comet tails and planetary rings, aiding our understanding of their production and evolution.