Description
We describe the formation of cool loops and the interaction of kink oscillations in coronal loop strands using magnetohydrodynamic simulation in ideal and non-ideal plasma regime. Firstly, we study the formation of cool loops using 2.5-dimensional MHD simulations in both adiabatic and non-adiabatic regimes. By implementing multiple transverse pulses resembling Alfvén pulses, we observe the non-linear transfer of energy and momentum to field-aligned perturbations through the ponderomotive force. This results in the creation of magnetoacoustic shocks and subsequent plasma motion, forming a cool loop system in the model solar atmosphere. We also examine the periodicity of flow velocity, applied Alfvén wave energy, and kinetic energy density along these cool loops, suggesting that impulsive Alfvén pulses can play a role in formation of cool loop and transportation of energy into the lower solar corona. Secondly, we describe the interaction of kink oscillations in strands of fine-structured cool coronal loops with field-aligned flows using 2-dimensional simulations under the ideal MHD regime. We investigate the influence of both uniform and non-uniform flow profiles on the characteristics of kink waves. We examine the excitation and attenuation of impulsively triggered fast magnetosonic standing kink waves, incorporating observed flow values by Hinode/SOT. We consider two types of inhomogeneity in longitudinal flow, varying in longitudinal and transverse directions. Our analysis under isobaric and isothermal conditions shows that the damping time decreases with increasing inhomogeneous flow width. The rate of damping-time reduction with respect to the half-width of flow is greater in unbounded flows compared to bounded flows.
