Resistive Tearing Instability in Electron-MHD: Application to Neutron Star Crusts

TL;DR

This paper investigates the resistive tearing instability in Electron-MHD, demonstrating its growth, nonlinear development, and potential impact on magnetic field evolution and heating in neutron star crusts, with broader implications for plasma systems.

Contribution

It provides a detailed analysis of the tearing instability in Electron-MHD, including linear growth rates, nonlinear simulations, and astrophysical implications for neutron star crusts.

Findings

Growth rate scales as γ ∝ B^{2/3} σ^{-1/3}

Formation of magnetic islands and X-points during instability

A small current sheet can release 10^{42} erg in days

Abstract

We study a resistive tearing instability developing in a system evolving through the combined effect of Hall drift in the Electron-MHD limit and Ohmic dissipation. We explore first the exponential growth of the instability in the linear case and we find the fastest growing mode, the corresponding eigenvalues and dispersion relation. The instability growth rate scales as $\gamma \propto B^{2/3} \sigma^{-1/3}$ where $B$ is the magnetic field and $\sigma$ the electrical conductivity. We confirm the development of the tearing resistive instability in the fully non-linear case, in a plane parallel configuration where the magnetic field polarity reverses, through simulations of systems initiating in Hall equilibrium with some superimposed perturbation. Following a transient phase, during which there is some minor rearrangement of the magnetic field, the perturbation grows exponentially. Once the instability is fully developed the magnetic field forms the characteristic islands and X-type reconnection points, where Ohmic decay is enhanced. We discuss the implications of this instability for the local magnetic field evolution in neutron stars' crusts, proposing that it can contribute to heating near the surface of the star, as suggested by models of magnetar post-burst cooling. In particular, we find that a current sheet a few meters thick, covering as little as $1\%$ of the total surface can provide $10^{42}~$erg in thermal energy within a few days. We briefly discuss applications of this instability in other systems where the Hall effect operates such as protoplanetary discs and space plasmas.