Rayleigh-Taylor instability in Magnetohydrodynamic Simulations of the Crab Nebula

TL;DR

This study uses high-resolution MHD simulations to analyze the development and behavior of Rayleigh-Taylor filaments in the Crab Nebula, revealing that magnetic tension does not prevent filament growth.

Contribution

It provides the first detailed axisymmetric simulation analysis showing magnetic tension's limited role in suppressing RT filaments in PWN.

Findings

Filaments are shaped by turbulent flow and hierarchical growth.

Magnetic dissipation leads to field-randomization, not suppression.

Results align with observed prominent filaments in Crab Nebula.

Abstract

In this paper we discuss the development of Rayleigh-Taylor filaments in axisymmetric simulations of Pulsar wind nebulae (PWN). High-resolution adaptive mesh refinement magnetohydrodynamic (MHD) simulations are used to resolve the non-linear evolution of the instability. The typical separation of filaments is mediated by the turbulent flow in the nebula and hierarchical growth of the filaments. The strong magnetic dissipation and field-randomization found in recent global three-dimensional simulations of PWN suggests that magnetic tension is not strong enough to suppress the growth of RT filaments, in agreement with the observations of prominent filaments in the Crab nebula. The long-term axisymmetric results presented here confirm this finding.