Three-dimensional numerical simulations of the pulsar magentoshere: Preliminary results

TL;DR

This paper presents three-dimensional, time-dependent numerical simulations of pulsar magnetospheres using a novel force-free electrodynamics solver, achieving steady-state solutions and enabling future detailed studies.

Contribution

Development of a new Eulerian finite difference time domain solver for force-free electrodynamics applied to pulsar magnetospheres.

Findings

Established a steady-state, quasi-stationary magnetosphere pattern.

Validated results with previous numerical solutions.

Enabled future high-resolution studies of dissipation and particle acceleration.

Abstract

We investigate the three-dimensional structure of the pulsar magnetosphere through time-dependent numerical simulations of a magnetic dipole that is set in rotation. We developed our own Eulerian finite difference time domain numerical solver of force-free electrodynamics and implemented the technique of non-reflecting and absorbing outer boundaries. This allows us to run our simulations for many stellar rotations, and thus claim with confidence that we have reached a steady state. A quasi-stationary corotating pattern is established, in agreement with previous numerical solutions. We discuss the prospects of our code for future high-resolution investigations of dissipation, particle acceleration, and temporal variability.