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D. Patnaude, R. Fesen (Dartmouth)
We present an analysis of the prominent bow shock-like feature (`Feature C') visible in both X-rays and radio synchrotron emission along the outer, northern shock boundary of the Cassiopeia A supernova remnant. Proper motion measurements using 2000 and 2004 Chandra X-ray image data of the bright emission knot at the leading edge of this apparent bow shock structure indicate a transverse velocity of 11000 ± 2000 km s-1. This is significantly larger than the 5000 - 6500 km s-1 velocity of the X-ray emitting forward shock front in this region of the remnant. We also present the X-ray spectrum of the bow shock's bright knot and compare it to spectra of neighboring sections of the forward shock. We will also show dynamical model results of ejecta `bullets' interacting with the forward and reverse shock fronts as well as local ISM/CSM clouds in order to simulate the observed bow shock structure.
This research was funded by the Chandra X-ray Observatory through the Archival Research Award AR4-5005X.
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Bulletin of the American Astronomical Society, 36 5
© 2004. The American Astronomical Society.