Astronomy and Astrophysics – Astronomy
Scientific paper
Aug 2004
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004head....8.2429b&link_type=abstract
American Astronomical Society, HEAD meeting #8, #24.29; Bulletin of the American Astronomical Society, Vol. 36, p.953
Astronomy and Astrophysics
Astronomy
Scientific paper
We present observations with the Chandra X-Ray Observatory of the supernova remnant 0049-73.6 in the Small Magellanic Cloud (SMC). In addition to the outer shell of the swept-up SMC gas, a bright ejecta dominated-ring is present in the remnant's interior. X-ray spectrum of the outer shell shows normal SMC abundances, and allows us to estimate the current blast wave speed at 600 km s-1. The swept-up mass is equal to 160 M&sun;, the SNR age is 16,000 yr, and the explosion energy is 8 × 1050 ergs. The brightest parts of the inner ring are dominated by O- and Ne-rich heavy-element ejecta. 0049-73.6 is thus a remnant of a core-collapse explosion. More diffuse interior ejecta emission shows less prominent O and Ne lines. We performed 1-D hydrodynamical simulations in order to understand the spatial structure of 0049-73.6. We identify the bright inner ring with a dense shell of ejecta interior to the contact discontinuity separating the shocked SMC gas and the SN ejecta. The reverse shock itself might might have already propagated into the low-density innermost ejecta. The observed location of the bright ring allows us to set up an upper limit of about 7-8 M&sun; of SN ejecta. The total mass of O within heavy-element ejecta is about 0.2--0.3 M&sun;. The filling fraction of the O-rich gas is less than 1%, and its high ionization state suggests that the observed emission is dominated by the dense ejecta clumps. The progenitor mass is estimated at about 10 M&sun;. It is likely that the progenitor star was a red supergiant star such as seen in a recent Type II-plateau SN 2003gd.
Borkowski Kazimierz J.
Hendrick Sean Patrick
Reynolds Stephen P.
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