Abstract:
The effects of solar activities on earth’s atmosphere, including coronal mass ejections and solar
wind, are critical for understanding the potential impacts on the planet’s magnetosphere,
including the ionosphere and exosphere. This thesis aims to investigate the effects of these solar
phenomena on Earth’s atmosphere by modeling the interaction of CME magnetic fields and solar
wind with Earth’s magnetic field. We employ numerical solution analysis using Finite Difference
Methods (FDM) to examine the evolutions of CME’s magnetic fields and the acceleration of
charged particles. The governing equations for this system are formulated, considering
disturbances to earth’s magnetic field caused by solar activities. We quantify the evolution of CME
magnetic fields and their interaction with Earth’s magnetosphere under various conditions, using
numerical solutions to the MHD induction equation. We also compare these results with
observational data to validate the model, focusing on parameters such as magnetic field null point,
breaking time and polarity changes. In our model, we assume the neglect of gravity, viscosity and
collisions for simplicity. As the result in particular, we derived the numerical solution for
convective, for diffusion and for general induction equations. The study provides insights into the
dynamics of solar wind and CMEs and their impact on Earth’s magnetic environment. Finally, we
compare the numerical solutions with observational data.
