Investigating the Structure of Vela X

TL;DR

This study uses X-ray observations and simulations to analyze Vela X, revealing complex ejecta structures, spectral variations, and the influence of the supernova remnant's reverse shock on its morphology.

Contribution

It provides detailed spectral analysis and hydrodynamical modeling of Vela X, enhancing understanding of its structure and evolution in the context of supernova remnant interactions.

Findings

Ejecta material confirmed within Vela X.

Temperature maps show low-temperature regions dominated by SNR emission.

Spectral variations indicate nonthermal emission concentrated near the pulsar.

Abstract

Vela X is the prototypical example of a pulsar wind nebula whose morphology and detailed structure have been affected by the interaction with the reverse shock of its host supernova remnant. The resulting complex of filamentary structure and mixed-in ejecta embedded in a nebula that is offset from the pulsar provides the best example we have of this middle-age state that characterizes a significant fraction of composite SNRs, and perhaps all of the large-diameter PWNe seen as TeV sources. Here we report on an XMM-Newton Large Project study of Vela X, supplemented by additional Chandra observations. Through broad spectral modeling as well as detailed spectral investigations of discrete emission regions, we confirm previous studies that report evidence for ejecta material within Vela X, and show that equivalent width variations of O VII and O VIII are consistent with temperature maps within the PWN that show low-temperature regions where the projected SNR emission appears to dominate emission from the ejecta. We identify spectral variations in the nonthermal emission, with hard emission being concentrated near the pulsar. We carry out investigations of the Vela X "cocoon" structure and, with hydrodynamical simulations, show that its overall properties are consistent with structures formed in the late-phase evolution of a composite SNR expanding into a surrounding medium with a density gradient, with ejecta material being swept beyond the pulsar and compressed into an elongated structure in the direction opposite the high external density.