Astronomy and Astrophysics – Astronomy
Scientific paper
Dec 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...21114404b&link_type=abstract
American Astronomical Society, AAS Meeting #211, #144.04; Bulletin of the American Astronomical Society, Vol. 39, p.997
Astronomy and Astrophysics
Astronomy
Scientific paper
We present an analysis of Chandra data on the pulse-quiet supernova remnant (SNR) MSH 11-62. The central region is dominated by non-thermal emission consistent with the presence of a pulsar wind nebula (PWN). Our spatial and spectral analysis strongly suggests the presence of a compact object with an inferred spin-down luminosity sufficient to power the nebula. Nebular asymmetry strongly suggests disruption by the SNR reverse shock and the nebula and SNR are consistent with being in pressure equilibrium. Thus, this observation provides evidence that, in this case, the ISM has had a dynamical effect on the SNR/PWN system. In order to explore the potential influence of the ISM on PWNe morphology, we have applied an existing adaptive-mesh, axisymmetric, relativistic hydrodynamic code to the simulation of the interaction of a relativistic pulsar wind with the slow, dense ambient flow setup by the space motion of the pulsar. We discuss simulations showing that this interaction can give rise to Guitar-like asymmetry leading to the formation of a relativistic backflow harboring a series of internal shocks. Further, we present the first results from an extension of the model to study the shock acceleration, and subsequent synchrotron cooling, of particles advected by the flow. The new module may be used to compute models of synchrotron emissivity and provides an energy sink, allowing for the exploration of the role of cooling on the flow dynamics. This work was supported by a NASA Graduate Student Researchers Program grant.
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