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

Journal Article · Sat Nov 10 00:00:00 EST 2012 · Astrophysical Journal

DOI:https://doi.org/10.1088/0004-637X/759/2/123· OSTI ID:22086358

Seward, F D ^[1]; Charles, P A ^[2]; Foster, D L ^[3]; Dickel, J R; Romero, P S ^[4]; Edwards, Z I; Perry, M; Williams, R M ^[5]

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1. Smithsonian Astrophysical Observatory, 60 Garden Street, Cambridge, MA 02138 (United States)
2. School of Physics and Astronomy, University of Southampton, Highfield, Southampton SO17 1BJ (United Kingdom)
3. South African Astronomical Observatory, P.O. Box 9, Observatory 7935, Cape Town (South Africa)
4. Department of Physics and Astronomy, University of New Mexico, 1919 Lomas Boulevard NE, Albuquerque, NM 87131 (United States)
5. Department of Earth and Space Sciences, Columbus State University, Coca Cola Space Science Center, 701 Front Avenue, Columbus, GA 31901 (United States)

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 {sub Sun}.

• OSTI ID: 22086358
• Journal Information: Astrophysical Journal, Vol. 759, Issue 2; Other Information: Country of input: International Atomic Energy Agency (IAEA); ISSN 0004-637X
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTROPHYSICS
COSMOLOGY AND ASTRONOMY
ASTROPHYSICS
BINARY STARS
COSMIC X-RAY SOURCES
DENSITY
GAMMA ASTRONOMY
MAGELLANIC CLOUDS
MASS
PHOTON EMISSION
PRECURSOR
STAR ACCRETION
SUPERNOVA REMNANTS
X RADIATION