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SN 1996cr, located in the Circinus Galaxy (3.7 Mpc, z ~ 0.001) wasnon-detected in X-rays at ~ 1000 days yet brightened to ~ 4 x 10^{39} erg/s(0.5-8 keV) after 10 years (Bauer et al. 2008). A 1-D hydrodynamic model of theejecta-CSM interaction produces good agreement with the measured X-ray lightcurves and spectra at multiple epochs. We conclude that the progenitor of SN1996cr could have been a massive star, M > 30 M_solar, which went from an RSGto a brief W-R phase before exploding within its ~ 0.04 pc wind-blown shell(Dwarkadas et al. 2010). Further analysis of the deep Chandra HETG observationsallows line-shape fitting of a handful of bright Si and Fe lines in thespectrum. The line shapes are well fit by axisymmetric emission models with anaxis orientation ~ 55 degrees to our line-of-sight. In the deep 2009 epoch thehigher ionization Fe XXVI emission is constrained to high lattitudes: theOccam-est way to get the Fe H-like emission coming from high latitude/polarregions is to have more CSM at/around the poles than at mid and lowerlattitudes, along with a symmetric ejecta explosion/distribution. SimilarCSM/ejecta characterization may be possible for other SNe and, withhigher-throughput X-ray observations, for gamma-ray burst remnants as well.

Modeling SN 1996cr's X-ray lines at high-resolution: Sleuthing the ejecta/CSM geometry