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tokens: and magnetic reconnections. By sampling the shock profiles at different times and different locations of the bow shock and tracing the particles, we have shown the following results: 1. We identify different stages in the macroscopic evolution of the bow shock and the entire formation of the magnetosphere in the meridian plane. The macrostructures reach a quasi-stable state after several ion cyclotron cycles, consistent with previous 3D implicit PIC simulations (Peng et al. 2015b ). Furthermore, a relatively high temporal-spatial resolution employed in our simulation provides an opportunity to examine the microstructure of the bow shock and the magnetic reconnection. 2. In the southward IMF condition, the shock around the subsolar point is quasi-perpendicular, and the shock at the wings is oblique. The angle and solar wind speed along the shock normal decrease with the distance away from the subsolar point. At quasi-perpendicular regions of the shock, a self-reformation of the shock front is found and the cyclic period of the reformation is similar to those observed in 1D and 2D local simulations. At the oblique region, the shock becomes weak due to the slow solar wind speed in the shock normal direction. 3. Different from 1D and 2D local simulations, particles in the downstream region are more complicated at the bow shock. By tracing the ions and electrons in the simulation, we find that the solar wind ions injected at the subsolar point will become diffuse and can be convected to the cusp region and the downstream of the oblique region of the bow shock. Electrons are more diffusive than ions in the downstream region. The ions injected at the northern part of the bow shock will fill in the northern part of the magnetosheath. A fraction of electrons injected at the same place will be convected to the southern part of the magnetosheath. The particles injected and reflected by the quasi-perpendicular shock region can affect the local velocity distributions and electromagnetic fluctuations in the transition and downstream regions of the oblique shock at the wings of the bow shock. This feature makes the oblique shock regions become a little different from those observed in local planar shock simulations. 4. The impact of the upstream plasma beta β i and solar wind Mach number M A on the bow shock and the magnetosphere show that the shock front becomes quasi-stationary in the high beta and low Mach number cases. In addition, the magnetotail reconnection disappears in this quasi-stationary case due to the low compression of the magnetotail under a low solar wind pressure condition. If we keep the Mach number of the incident solar wind unchanged and only increase the beta value, the bow shock is still nonstationary. Contrasting the low beta case, the ripple scale becomes larger in the high beta case. 5. To confirm the impact of the solar wind condition on the bow shock front nonstationarity, we also studied the time evolution of shock