Investigation of Kelvin-Helmholtz instability during the reconnection process in the solar atmosphere

This project aims to study the Kelvin-Helmholtz instability (KHI) as a possible mechanism for the formation of plasma escape during the reconnection process in the solar atmosphere. The KHI is formed with a continuous profile through the interface of two viscous fluid layers. We investigate the effects of wavenumber, shear rate, magnetic field, and temperature on the growth rate of magnetized KHI. The Magnetohydrodynamic equations describing the momentum, mass, energy conservations, and magnetic induction for incompressible plasma are applied to viscous and non-viscous cases.