@article{slane_lovchinsky_kolb_snowden_temim_blondin_bocchino_miceli_chevalier_hughes_et al._2018, title={Investigating the Structure of Vela X}, volume={865}, ISSN={["1538-4357"]}, url={https://doi.org/10.3847/1538-4357/aada12}, DOI={10.3847/1538-4357/aada12}, abstractNote={Abstract Vela X is a prototypical example of a pulsar wind nebula whose morphology and detailed structure have been affected by 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 supernova remnants (SNRs), and perhaps all of the large-diameter pulsar wind nebulae (PWNe) seen as TeV sources. Here, we report on an XMM-Newton (hereafter XMM) 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.}, number={2}, journal={ASTROPHYSICAL JOURNAL}, author={Slane, P. and Lovchinsky, I and Kolb, C. and Snowden, S. L. and Temim, T. and Blondin, J. and Bocchino, F. and Miceli, M. and Chevalier, R. A. and Hughes, J. P. and et al.}, year={2018}, month={Oct} } @article{kolb_blondin_slane_temim_2017, title={Evolution of a pulsar wind nebula within a composite supernova remnant}, volume={844}, number={1}, journal={Astrophysical Journal}, author={Kolb, C. and Blondin, J. and Slane, P. and Temim, T.}, year={2017} } @article{temim_slane_plucinsky_gelfand_castro_kolb_2017, title={Proper Motion of the High-velocity Pulsar in SNR MSH 15-56}, volume={851}, ISSN={["1538-4357"]}, DOI={10.3847/1538-4357/aa9d41}, abstractNote={Abstract We present a measurement of the proper motion of the presumed pulsar in the evolved composite supernova remnant (SNR) MSH 15-56 whose pulsar wind nebula (PWN) has been disrupted by the supernova (SN) reverse shock. Using Chandra X-ray observations acquired over a baseline of 15 years, we measure a pulsar velocity of and a direction of motion of 14° ± 22° west of south. We use this measurement to constrain a hydrodynamical (HD) model for the evolution of this system, and find that its morphology is well-described by an SNR expanding in an ambient density gradient that increases from east to west. The effect of the density gradient and the pulsar’s motion is an asymmetric interaction between the SN reverse shock and the PWN that displaces the bulk of the PWN material away from the pulsar toward the northeast. The simulation is consistent with an SNR age of 11,000 years, an SN ejecta mass of 10 M ⊙, and an average surrounding density of 0.4 cm−3, but a combination of a higher SN ejecta mass and ambient density can produce a similar SNR morphology at a later age.}, number={2}, journal={ASTROPHYSICAL JOURNAL}, author={Temim, Tea and Slane, Patrick and Plucinsky, Paul P. and Gelfand, Joseph and Castro, Daniel and Kolb, Christopher}, year={2017}, month={Dec} } @article{temim_slane_kolb_blondin_hughes_bucciantini_2015, title={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}, volume={808}, number={1}, journal={Astrophysical Journal}, author={Temim, T. and Slane, P. and Kolb, C. and Blondin, J. and Hughes, J. P. and Bucciantini, N.}, year={2015} }