An Fe-Ni Bubble in the Small Magellanic Cloud Supernova Remnant B0049-73.6

Details An Fe-Ni Bubble in the Small Magellanic Cloud Supernova Remnant B0049-73.6 An Fe-Ni Bubble in the Small Magellanic Cloud Supernova Remnant B0049-73.6

Apr 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005apj...622l.117h&link_type=abstract

The Astrophysical Journal, Volume 622, Issue 2, pp. L117-L120.

Astronomy and Astrophysics

Astronomy

11

Ism: Individual: Alphanumeric: B0049-73.6, Ism: Supernova Remnants, X-Rays: Ism

Scientific paper

We present observations with the Chandra X-Ray Observatory of the supernova remnant (SNR) B0049-73.6 in the Small Magellanic Cloud (SMC). The remnant shows outer emission from swept-up SMC gas and a bright ejecta-dominated ring in the interior. The X-ray spectrum of the outer shell shows normal SMC abundances and allows us to estimate the current blast wave speed at 570 km s-1 from Sedov models. The swept-up mass is equal to 170 Msolar, the SNR age is 14,000 yr, and the explosion energy is 8.1×1050 ergs. The brightest parts of the inner ring are dominated by O- and Ne-rich heavy-element ejecta. B0049-73.6 is thus a remnant of a core-collapse explosion. More diffuse interior ejecta emission shows less prominent O and Ne lines. The total mass of O within the heavy-element ejecta is about 0.3 Msolar. The filling fraction of the O-rich gas is less than 1%, and its average ionization timescale of 5×1010 cm-3 s suggests that the observed emission is dominated by relatively dense (ne~0.2 cm-3) ejecta. The bright inner ring most likely is composed of the innermost ejecta swept up by a central ``nickel bubble'' resulting from radioactive energy input from freshly synthesized 56Ni. This is in a qualitative agreement with theoretical predictions of such centrally located Fe-Ni bubbles, and it confirms the important role of the Ni bubble effect in determining the innermost ejecta structure in core-collapse supernovae.

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