Speaker
Description
We present an interactive 3D Particle-In-Cell (PIC) simulation of a global pulsar magnetosphere implemented in a browser-based HTML/WebGL environment. The model self-consistently evolves electromagnetic fields and relativistic plasma by solving Maxwell’s equations on a discretized grid (Yee scheme) coupled to particle dynamics via the Lorentz force. Charged particles are advanced using a relativistic Boris pusher, while charge and current densities are deposited onto the grid to ensure consistent field–particle coupling.
The simulation captures key physical processes of pulsar magnetospheres, including rotation-induced electric fields, charge separation, current closure, and the formation of equatorial current sheets near the light cylinder. Pair injection is modeled through parameterized source terms to approximate cascade processes in the open-field-line region. A dipolar magnetic field anchored to a rotating neutron star provides the global structure, enabling exploration of aligned and oblique rotator configurations.
Although limited in resolution compared to large-scale HPC PIC codes, the implementation preserves the essential kinetic and electrodynamic behavior reported in the literature. The interactive interface exposes physically meaningful parameters—such as rotation rate, magnetic field strength, obliquity, and pair production rate—allowing users to investigate transitions between vacuum, charge-separated, and quasi force-free regimes. This work aims to provide a scientifically grounded, accessible platform for both education and rapid conceptual exploration in computational astrophysics.