Time evolution of pulsar obliquity angle from 3D simulations of magnetospheres

Abstract

The rotational period of isolated pulsars increases over time due to the extraction of angular momentum by electromagnetic torques. These torques also change the obliquity angle $α$ between the magnetic and rotational axes. Although actual pulsar magnetospheres are plasma-filled, the time evolution of $α$ has mostly been studied for vacuum pulsar magnetospheres. In this work, we self-consistently account for the plasma effects for the first time by analysing the results of time-dependent 3D force-free and magnetohydrodynamic simulations of pulsar magnetospheres. We show that if a neutron star is spherically symmetric and is embedded with a dipolar magnetic moment, the pulsar evolves so as to minimise its spin-down luminosity: both vacuum and plasma-filled pulsars evolve toward the aligned configuration ($α=0$). However, they approach the alignment in qualitatively different ways. Vacuum pulsars come into alignment exponentially fast, with $α\propto \exp(-t/τ)$ and $τ\sim$ spindown timescale. In contrast, we find that plasma-filled pulsars align much more slowly, with $α\propto (t/τ)^{-1/2}$. We argue that the slow time evolution of obliquity of plasma-filled pulsars can potentially resolve several observational puzzles, including the origin of normal pulsars with periods of $\sim1$ second, the evidence that oblique pulsars come into alignment over a timescale of $\sim 10^7$ years, and the observed deficit, relative to an isotropic obliquity distribution, of pulsars showing interpulse emission.