G337.2-0.7: an Asymmetric Type Ia Supernova Remnant?

Details G337.2-0.7: an Asymmetric Type Ia Supernova Remnant? G337.2-0.7: an Asymmetric Type Ia Supernova Remnant?

Aug 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004head....8.2425r&link_type=abstract

American Astronomical Society, HEAD meeting #8, #24.25; Bulletin of the American Astronomical Society, Vol. 36, p.953

Astronomy and Astrophysics

Astronomy

Scientific paper

The ASCA X-ray spectrum of supernova remnant (SNR) G337.2-0.7 showed strong X-ray emission lines, proving the remnant to be young and dominated by supernova ejecta. Its combination of high abundances in the intermediate mass elements from Si to Ca and an a-spherical morphology make it an interesting test case for supernova models. We have followed up on this result with deeper observations using XMM and Chandra. These new data show that the abundance ratios from Ne to Fe are far from solar, with little evidence for Fe-K emission, and a Ca to Si ratio that is at least 3.1 times their solar ratio at the 99% confidence. Comparing these abundances with the total production factors of a wide range of core-collapse and type Ia models, we find that it is difficult to achieve such a non-solar abundance pattern of Si, S, Ar and Ca in a core-collapse model. Although a 12 M&sun; model by Woosley & Weaver 1995 cannot be ruled out, a delayed detonation type Ia model is more plausible. Furthermore, comparisons of the overall SNR spectrum with the X-ray emission from the remnant of a type Ia SN calculated by Badenes et al. (2003), show that a delayed detonation model may be a promising explosion mechanism. It qualitatively reproduces the continuum temperature, the absolute and relative abundances of Ne, Mg, Si, S, Ca, and Fe, and the ionization states of Si and S of G337.2-0.7 remarkably well at a reasonable age for the remnant.
C. Rakowski acknowledges support for this work from NASA GXXXXX.

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