The interaction of the solar wind with the terrestrial magnetosphere is analyzed with the help of three‐dimensional (3‐D) global, full‐electromagnetic particle‐in‐cell (PIC) simulations, in the configuration where the interplanetary magnetic field (IMF) is steadily northward. The present study is mainly focused on the cusp region and associated particle momenta dynamics. Within the present context and to the best of our knowledge, this work represents the first numerical simulation for analyzing the cusp dynamics using a fully self‐consistent 3‐D kinetic and electromagnetic approach. The main goals of the study are the following: (i) to retrieve the main known features of the cusp to validate the use of 3‐D PIC “global” simulations, (ii) to compare with previous results obtained with 3‐D MHD simulations, (iii) to create an updated global view of the cusp based on use of 3‐D PIC simulation, which cannot be obtained from a MHD approach, and (iv) to compare with statistical results from the Cluster mission. In particular, the stagnant exterior cusp (SEC) identified in previous statistical analysis of experimental data is retrieved, and it is possible to more precisely define the edges of the SEC region. In addition, we will focus on cusp features recently observed by the Cluster mission, for example, the Alfvén Transition Layer or ATL and on the features not reproduced by either MHD or the hybrid approach, which have been used to characterize the outer edges of the cusp more clearly.

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Magnetosonic waves are studied in the presence of degenerate pressure due to Landau diamagnetic levels and Pauli spin magnetization with strong magnetic field in quantum degenerate electron-ion plasma. A linear dispersion relation of low frequency propagation wave in the direction of magnetic field is derived that strongly depends on the magnetic field while in classical regime this field has no such a role. In the presence of quantization of orbital motion and spin magnetization, new propagation modes of quantum plasmas are also explored. It is noted that quantum acoustic velocity and spin magnetization energy affect the Alfven mode propagation. The quantum effects are incorporated through the Bohm potential, Landau pressure due to Landau quantization of magnetic field and magnetization energy due to spin effect. The current model in the context of Landau diamagnetic pressure along with spin magnetization is sufficient for studying the astrophysical plasma environment existing in the compact systems e.g., white dwarfs and neutron stars.and while the field of interior core of NS can reach ;10 11 Tesla or even may be higher [9][10][11]. Further this field may be increased by a factor 10 3 ∼10 4 due to the rotational movement of stars RECEIVED

The energetic charged particles penetration in the plasmasphere are carried out using the updated version of 3D Stanford PIC code. We considered slow and fast wind streams to know the penetration of the energetic charged particles (electrons and ions) having different velocities into four regions i.e. cusp, plasmasphere, sunward, and tailward sides. It is observed that the ion penetrations are higher than electrons for solar slow wind streams in the plasmasphere, while it is reverse for the solar fast streams. Also, the results show that the percentage of penetration of the energetic charged particles (both electrons and ions) are the same into the cusp and subsolar point reconnection region. It is different for the higher speed of fast streams; so that the penetrated electrons reached about 10–20 times than penetrated ions. The results show that for the tailward reconnection region, the penetration of ions is 2–3 times higher than the penetration of electrons, but it is the same for the case of higher solar fast speed.

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