Diffusivity in force-free simulations of global magnetospheres

TL;DR

This study investigates how numerical diffusivity in force-free simulations affects pulsar magnetosphere dynamics, revealing that reduced diffusivity leads to increased luminosity and shifts in the Y-point, with implications for understanding resistivity and pair formation.

Contribution

It introduces a comparison of techniques to model charge density, showing how different approaches influence magnetospheric dynamics and pulsar luminosity in force-free simulations.

Findings

Reducing numerical diffusivity decreases Poynting flux dissipation.

Luminosity scales with diffusion-to-advection timescale ratio as L_Y ∝ α^{0.11}.

Different charge density modeling approaches significantly impact simulation outcomes.

Abstract

Abstract: Assuming that the numerical diffusivity triggered by violations of the force-free electrodynamics constraints is a proxy for the physical resistivity, we examine its impact on the overall dynamics of force-free aligned pulsar magnetospheres endowed with an equatorial current sheet. We assess the constraint violations as a diffusivity source. The effects of modifications on electric fields used to restore force-free conditions are not confined to the equatorial current sheet, but modify the magnetospheric dynamics on timescales shorter than the pulsar rotational period. These corrections propagate especially via a channel that was unexplored, namely, changes induced to the electric charge density, $\rho$. We quantify the global consequences of diffusivity by comparing different techniques to model $\rho$. By default, we combine a conservative $\rho$-evolution with hyperbolic/parabolic cleaning of inaccuracies in the Maxwell equations. As an alternative, we enforce a constrained evolution where $\rho$ is directly computed as the electric field divergence. The conservative approach reduces the Poynting flux dissipated in the equatorial current sheet by an order of magnitude, along with an increase of the pulsar luminosity driven by a shift of the Y-point location. The luminosity changes according to $L_{\rm Y}\propto \alpha^{0.11}$, where $\alpha$ is the ratio of diffusion to advection timescales, controlling the amount of (numerical) diffusivity. Our models suggest interpreting the luminosity dependence on the Y-point location as differences in resistivities encountered at the equatorial current sheet. Alternatively, they could be interpreted in terms of the pair formation multiplicity, $\kappa$, smaller diffusion being consistent with $\kappa\gg 1$.