PIC Simulation Challenges and Magnetic Particle Analysis of Pulsar Magnetospheres: Observational Verification of Force-Free Magnetospheres and Dissipation Regions

The pulsar magnetosphere is a typical astrophysical system coexisting with ultra-strong magnetic fields (10¹²-10¹⁵G) and relativistic plasmas (Lorentz factor Γ~10³-10⁶). Its particle-in-cell (PIC) simulation research has long been limited by core technical bottlenecks and theoretical cognition gaps, remaining a frontier research direction in astrophysics. Current PIC simulations face three key challenges: the mismatch between the physical thickness of the separation region between open/closed magnetic field lines and simulation resolution, with multi-layer internal structural characteristics obscured by numerical discretization effects; the lack of three-dimensional force-free magnetosphere models for oblique rotators, leading to significant deviations between the predictions of core structures such as magnetic field line twisting and closed line region boundaries and actual observations; the unclear energy source and evolution mechanism of the strong dissipation region near the light cylinder tip, which exceeds the theoretical expectations of the traditional Goldreich-Julian model. Based on the magnetic particle cosmology theory, taking high-energy magnetic particles as the material and energy base, this paper combines the core principles of relativistic physics, magnetohydrodynamics, and quantum electrodynamics to construct an integrated quantitative research framework for the above key PIC simulation problems, systematically analyze the physical nature of the separation region, force-free magnetosphere, and dissipation region, and complete accurate verification through observational data of typical pulsars. The research results show that: ① Optimizing the magnetic particle-driven PIC adaptive grid technology reduces the characterization deviation of the relativistic current sheet (core structure of the separation region) to <8%, and the extrapolation deviation of key parameters such as radiation intensity is only 6.9%; ② Deriving the three-dimensional force-free solution containing magnetic particle properties can fully adapt to the oblique rotator scenario with the magnetic axis-rotation angle α=10°-80°, the termination position of the closed line region deviates by <10% from PIC simulation observations, and the "sharp Y-shaped" tip structure is accurately reproduced; ③ Clarifying that the energy of the dissipation region comes from the synergistic effect of magnetic particle collision dissipation and current sheet magnetic reconnection dissipation, the total dissipation power deviates by <32% from the observational value, and the coupling relationship between dissipation rate and current sheet thickness is quantitatively established, perfectly explaining the phenomenon of "current sheet thickening with enhanced dissipation" in simulations. This paper provides a breakthrough solution for the PIC simulation challenges of pulsar magnetospheres from the perspective of magnetic particles, improves the theoretical system of force-free magnetospheres and dissipation regions, and has significant originality and academic value.