Iron-Rich Ejecta in the Supernova Remnant DEM L71

Details Iron-Rich Ejecta in the Supernova Remnant DEM L71 Iron-Rich Ejecta in the Supernova Remnant DEM L71

2002-12-05

arxiv.org/abs/astro-ph/0212118v1

Astrophys.J. 582 (2003) L95-L100

Astronomy and Astrophysics

Astrophysics

5 pages, including 3 postscript figs, LaTeX, to appear in ApJ Letters 2003 Jan 10

Scientific paper

10.1086/367760

Chandra X-ray observations of DEM L71, a supernova remnant (SNR) in the Large Magellanic Cloud (LMC), reveal a clear double shock morphology consisting of an outer blast wave shock surrounding a central bright region of reverse-shock heated ejecta. The abundances of the outer shock are consistent with LMC values, while the ejecta region shows enhanced abundances of Si, Fe, and other species. However, oxygen is not enhanced in the ejecta; the Fe/O abundance ratio there is more than 5 times the solar ratio. Based on the relative positions of the blast wave shock and the contact discontinuity in the context of SNR evolutionary models, we determine a total ejecta mass of approximately 1.5 solar masses. Ejecta mass estimates based on emission measures derived from spectral fits are subject to considerable uncertainty due to lack of knowledge of the true contribution of hydrogen continuum emission. Maximal mass estimates, i.e., assuming no hydrogen, result in 1.5 solar masses of Fe and 0.24 solar masses of Si. Under the assumption that an equal quantity of hydrogen has been mixed into the ejecta, we estimate 0.8 solar masses of Fe and 0.12 solar masses of Si. These characteristics support the view that in DEM L71 we see Fe-rich ejecta from a Type Ia SN several thousand years after explosion.

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