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In an effort to better understand the evolution of composite supernovaremnants (SNRs) and the eventual fate of relativistic particles injected bytheir pulsars, we present a multifaceted investigation of the interactionbetween a pulsar wind nebula (PWN) and its host SNR G327.1-1.1. Our 350 ksChandra X-ray observations of SNR G327.1-1.1 reveal a highly complexmorphology; a cometary structure resembling a bow shock, prong-like featuresextending into large arcs in the SNR interior, and thermal emission from theSNR shell. Spectral analysis of the non-thermal emission offers clues about theorigin of the PWN structures, while enhanced abundances in the PWN regionprovide evidence for mixing of supernova ejecta with PWN material. The overallmorphology and spectral properties of the SNR suggest that the PWN hasundergone an asymmetric interaction with the SNR reverse shock (RS) that canoccur as a result of a density gradient in the ambient medium and/or a movingpulsar that displaces the PWN from the center of the remnant. We presenthydrodynamical simulations of G327.1-1.1 that show that its morphology andevolution can be described by a ~ 17,000 yr old composite SNR that expandedinto a density gradient with an orientation perpendicular to the pulsar'smotion. We also show that the RS/PWN interaction scenario can reproduce thebroadband spectrum of the PWN from radio to gamma-ray wavelengths. The analysisand modeling presented in this work have important implications for our generalunderstanding of the structure and evolution of composite SNRs.

astrophysical journal/the astrophysical journal

Late-time Evolution of Composite Supernova Remnants: Deep Chandra  Observations and Hydrodynamical Modeling of a Crushed Pulsar Wind Nebula in  SNR G327.1-1.1