A Chandra X-ray Study of Supernova Remnant N63A in the Large Magellanic Cloud

Abstract

We perform extensive spectroscopy of the supernova remnant N63A in the Large Magellanic Cloud, using $\sim 43$ ks {\it Chandra} archival data. By analysing the spectra of the entire remnant, we determine the abundance distributions for O, Ne, Mg, Si, and Fe. We detect evidence of enhanced O and possibly Ne and Mg in some of the central regions which might indicate an asymmetric distribution of the ejecta. The average O/Ne, O/Mg, and Ne/Mg abundance ratios of the ejecta are in plausible agreement with the nucleosynthesis products from the explosion of a $\sim 40$ $M_{\odot }$ progenitor. We estimate an upper limit on the Sedov age of $\sim 5,400\pm 200$ yr and explosion energy of $\sim 8.9\pm 1.6\times 10^{51}$ erg for N63A. We discuss the implications of our results for the morphological structure of the remnant, its circumstellar medium and the nature of the progenitor star.

arXiv comment22 pages, including 9 figures and 4 tables, accepted for publication in Monthly Notices of the Royal Astronomical Society. arXiv admin note: substantial text overlap with arXiv:2201.09891

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Cited by in corpus (2)

• Chandra and XMM-Newton X-ray Study on the Core-collapse Supernova Remnant N63A in an H II Region
• Quantifying Symmetry: Transformation Information for Planetary Nebulae and Supernova Remnants