In the present paper, we have studied the nonlinear Kinetic Alfvén Waves (KAW) in the vicinity of the null point. We have considered the nonlinearity due to ponderomotive effects associated with KAW in the solar corona. A 3D model equation representing the dynamics of KAW is developed in this Null point scenario. Using numerical methods, we have solved the model equation for solar corona parameters. The pseudospectral method and the finite difference method have been applied to tackle spatial integration and temporal evaluation, respectively. The outcome of the simulation demonstrates the formation of localized structures. With the evolution of time, these localized structures become more chaotic. Chaotic structures (turbulent) can efficiently transfer energy. The power spectrum of these turbulent structures shows the Kolmogorov spectral index of nearly − 5 3 in the inertial range followed by a steeper spectrum of nearly −3.3 (in the range of −2 to −4). These structures also lead to the generation of the current sheet. To understand the physics of our model, we have also done a semi-analytical study for our model equation. Semi-analytical calculations reveal that the current sheet structures have scale sizes of the order of ion gyro-radius. The relevance of this investigation to the current observations by Parker Solar Probe has also been discussed.

In the present paper, we have studied the nonlinear Kinetic Alfv'en Waves (KAW) in the vicinity of the null point. We have considered the nonlinearity due to ponderomotive effects associated with KAW in the solar corona. A 3D model equation representing the dynamics of KAW is developed in this Null point scenario. Using numerical methods, we have solved the model equation for solar corona parameters. The pseudospectral method and the finite difference method have been applied to tackle spatial integration and temporal evaluation, respectively. The outcome of the simulation demonstrates the formation of localized structures. With the evolution of time, these localized structures become more chaotic. Chaotic structures (turbulent) can efficiently transfer energy. The power spectrum of these turbulent structures shows the Kolmogorov spectral index of nearly -5/3 in the inertial range followed by a steeper spectrum of nearly -3.3 (in the range of -2 to -4). These structures also lead to the generation of the current sheet. To understand the physics of our model, we have also done a semi-analytical study for our model equation. Semi-analytical calculations reveal that the current sheet structures have scale sizes of the order of ion gyro-radius. The relevance of this investigation to the current observations by Parker Solar Probe has also been discussed.