A Dual Attack: Pulsar Wind Nebulae Simulations and X-Ray Observations of MSH 11-62

Details A Dual Attack: Pulsar Wind Nebulae Simulations and X-Ray Observations of MSH 11-62 A Dual Attack: Pulsar Wind Nebulae Simulations and X-Ray Observations of MSH 11-62

Dec 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004aas...20510206b&link_type=abstract

American Astronomical Society Meeting 205, #102.06; Bulletin of the American Astronomical Society, Vol. 36, p.1512

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We present the results from a joint computational and observational study of the interaction of a light, relativistic pulsar wind with the dense, slow-moving ISM flow resulting from the space motion of the pulsar. Such a scenario has been suggested as the origin of asymmetric pulsar wind nebulae (PWNe). We discuss the application of an existing adaptive mesh, axisymmetric, relativistic hydrodynamic code to the simulation of such a flow, and in particular, the modification to the solver necessitated by the ultra relativistic nature of the pulsar wind. We present the analysis of a 50 kilosecond Chandra X-ray Observatory observation of the supernova remnant (SNR) MSH 11-62. We show that the spectrum of the central region of the SNR above 2 keV is dominated by non-thermal emission consistent with the presence of a PWN of angular radius ˜ 5 arcsec (implying a physical radius ˜ 0.1 pc at a distance of 3.5 kpc). Our spectral analysis implies the presence of a compact object with a spectral index Γ ˜ 1.3 and a spin-down energy ˙ {E} ˜ 1035 erg s-1, a value sufficient to conclude that the putative PWN is rotationally powered. Our timing analysis yields a null result and so pulses from the compact object remain undetected.

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