How Pulsars Shine: Poynting Flux Annihilation

TL;DR

This paper presents an exact analytical solution to pulsar equations in a simplified geometry, capturing key features like force-free zones and Poynting flux annihilation, improving understanding of pulsar emission mechanisms.

Contribution

It provides a simplified, exact analytical model of pulsar magnetospheres that reproduces essential features previously obtained through complex numerical simulations.

Findings

Exact solution reproduces force-free and radiation zones

Demonstrates Poynting flux annihilation into curvature radiation

Simplifies understanding of pulsar emission processes

Abstract

Recent solution of a pulsar (although likely correct, as agreeing with phenomenology of weak pulsars without a single adjustable) is somewhat unsatisfactory on account of being heavily numerical. Here the main features of a pulsar -- (i) the existence of a force-free zone, (ii) bounded by a non-force-free radiation zone, (iii) where colliding Poynting fluxes annihilate into curvature radiation -- are reproduced as an exact solution of the same pulsar equations but in a much simpler geometry.