Fast dissipation of Colliding Alfv\'en Waves in a Magnetically Dominated Plasma

TL;DR

This paper introduces a rapid magnetic energy dissipation mechanism via colliding Alfvén waves forming a current sheet, which can operate faster than traditional reconnection in magnetically dominated plasmas.

Contribution

The study demonstrates a new dissipation process involving wave collision and current sheet formation, with kinetic simulations showing its efficiency and transition to reconnection at high amplitudes.

Findings

Dissipation efficiency reaches 100% at wave amplitude A=1.

Mechanism activates when A>1/2, dissipating large wave energy.

Transition to magnetic reconnection occurs at high amplitudes A>>1.

Abstract

Magnetic energy around compact objects often dominates over plasma rest mass, and its dissipation can power the object luminosity. We describe a dissipation mechanism which works faster than magnetic reconnection. The mechanism involves two strong Alfv\'en waves with anti-aligned magnetic fields $\boldsymbol{B}_1$ and $\boldsymbol{B}_2$ that propagate in opposite directions along background magnetic field $\boldsymbol{B}_0$ and collide. The collision forms a thin current sheet perpendicular to $\boldsymbol{B}_0$, which absorbs the incoming waves. The current sheet is sustained by electric field $\boldsymbol{E}$ breaking the magnetohydrodynamic condition $E<B$ and accelerating particles to high energies. We demonstrate this mechanism with kinetic plasma simulations using a simple setup of two symmetric plane waves with amplitude $A=B_1/B_0=B_2/B_0$ propagating in a uniform $\boldsymbol{B}_0$. The mechanism is activated when $A>1/2$. It dissipates a large fraction of the wave energy, $f=(2A-1)/A^2$, reaching $100\%$ when $A=1$. The plane geometry allows one to see the dissipation process in a one-dimensional simulation. We also perform two-dimensional simulations, enabling spontaneous breaking of the plane symmetry by the tearing instability of the current sheet. At moderate $A$ of main interest the tearing instability is suppressed. Dissipation transitions to normal, slower, magnetic reconnection at $A\gg 1$. The fast dissipation described in this paper may occur in various objects with perturbed magnetic fields, including magnetars, jets from accreting black holes, and pulsar wind nebulae.