Ab-initio pulsar magnetosphere: three-dimensional particle-in-cell simulations of oblique pulsars

TL;DR

This study uses first-principles 3D particle-in-cell simulations to explore pair formation and magnetospheric structures in oblique pulsars, revealing how obliquity affects pair production and magnetic dissipation.

Contribution

It provides the first detailed relativistic PIC simulation of oblique pulsar magnetospheres including pair formation, highlighting the dependence on obliquity and revealing the structure of the current sheet.

Findings

Pair formation occurs mainly in the current sheet for low obliquity.

Higher obliquity leads to pair production in open field lines.

Magnetic dissipation varies with obliquity, from 20% to 3%.

Abstract

We present first-principles relativistic particle-in-cell simulations of the oblique pulsar magnetosphere with pair formation. The magnetosphere starts to form with particles extracted from the surface of the neutron star. These particles are accelerated by surface electric fields and emit photons capable of producing electron-positron pairs. We inject secondary pairs at locations of primary energetic particles, whose energy exceeds the threshold for pair formation. We find solutions that are close to the ideal force-free magnetosphere, with the Y-point and current sheet. Solutions with obliquities $\lt 40^{\circ}$ do not show pair production in the open field line region, because the local current density along magnetic field is below the Goldreich-Julian value. The bulk outflow in these solutions is charge separated, and pair formation happens in the current sheet and return current layer only. Solutions with higher inclinations show pair production in the open field line region, with high multiplicity of the bulk flow and the size of pair-producing region increasing with inclination. We observe the spin-down of the star to be comparable to MHD model predictions. The magnetic dissipation in the current sheet ranges between 20% for the aligned rotator and 3% for the orthogonal rotator. Our results suggest that for low obliquity neutron stars with suppressed pair formation at the light cylinder, the presence of phenomena related to pair activity in the bulk of the polar region, e.g., radio emission, may crucially depend on the physics beyond our simplified model, such as the effects of curved space-time or multipolar surface fields.