Modeling The Morphology Of SN 1996cr From X-ray Lines At High Resolution
Abstract
SN1996cr ( 3.7 Mpc) was X-ray "dim" up to 1000 days yet brightened to 4e39 erg/s (0.5-8 keV) after 10 years (Bauer et al. 2008). A 1-D hydro model of the ejecta-CSM interaction produces good agreement with the measured X-ray light curves and spectra at multiple epochs, suggesting that SN 1996cr was most likely a massive star, M > 30 solar masses, which went from an RSG to a brief W-R phase before exploding within its r 0.04 pc wind-blown shell (Dwarkadas et al. 2010). Further analysis of a 485ks Chandra HETG observation allows velocity-profile fitting to a handful of bright emission lines in the spectrum (e.g., Si and Fe). The line shapes are well fit with axisymmetric emission models that put the higher temperature Fe XXVI emission at high latitudes. The axis orientation is well constrained to be 55 degrees from our line-of-sight. The latitude variation may be explained either by higher CSM densities near the equator, or by the ejecta having greater velocity along the poles. SN1996cr demonstrates how X-ray emission lines can provide important diagnostics of SN shock structure.
- Publication:
-
American Astronomical Society Meeting Abstracts #217
- Pub Date:
- January 2011
- Bibcode:
- 2011AAS...21743426B