Rayleigh-Taylor instability in Magnetohydrodynamic Simulations of the 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.

Updated affiliations and acknowledgements, 13 pages, submitted to MNRAS

References in corpus (3)

• The Magnetic Rayleigh-Taylor Instability in Three Dimensions
• High-Altitude Emission from Pulsar Slot Gaps: The Crab Pulsar
• X-ray illumination of the ejecta of Supernova 1987A

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