DEM L241, A SUPERNOVA REMNANT CONTAINING A HIGH-MASS X-RAY BINARY

2012/08/07 by F. D. Seward, P. A. Charles, D. L. Foster +5
Physics and Astronomy · #Astronomy and Astrophysical Research #Astrophysical Phenomena and Observations #Binary star #Gamma-ray bursts and supernovae #Large Magellanic Cloud #Near-Earth supernova #Orbital period #Solar mass #Supernova #Supernova remnant #Thermal emission #astro-ph.HE

paper · pdf · doi:10.1088/0004-637x/759/2/123

arxiv created 2012/08/07 · openalex publication_date 2012/10/29 · arxiv updated 2015/06/11 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05

Abstract

A Chandra observation of the Large Magellanic Cloud supernova remnant DEM L241 reveals an interior unresolved source which is probably an accretion-powered binary. The optical counterpart is an O5III(f) star making this a high-mass X-ray binary with an orbital period likely to be of the order of tens of days. Emission from the remnant interior is thermal and spectral information is used to derive density and mass of the hot material. Elongation of the remnant is unusual and possible causes of this are discussed. The precursor star probably had mass >25 M ☉

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