Radio properties of three young supernova remnants in the Large Magellanic Cloud

Details Radio properties of three young supernova remnants in the Large Magellanic Cloud Radio properties of three young supernova remnants in the Large Magellanic Cloud

Jan 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995aj....109..200d&link_type=abstract

The Astronomical Journal (ISSN 0004-6256), vol. 109, no. 1669, p. 200-208

Astronomy and Astrophysics

Astronomy

24

Magellanic Clouds, Radio Astronomy, Radio Sources (Astronomy), Supernova Remnants, Astronomical Polarimetry, Balmer Series, H Ii Regions, Interstellar Magnetic Fields, Massive Stars, Oxygen

Scientific paper

Radio images of N132D, N103B, and 0519-690 have been made with the Australian Telescope. These three prominent young Supernova remnants (SNRs) in the Large Magellanic Cloud (LMC) have significantly different optical properties: N132D is oxygen rich and probably had a massive progenitor similar to Cas A; N103B, on the edge of a massive H II region complex, was probably also from a masssive star; on the other hand, isolated Balmer-dominated 0519-690 was probably from a low-mass Type Ia supernova. All three remnants show the characteristics shell structure with some clumpiness. Although the polarimetric data are not complete for all three, the results are compatible with a small net radial orientation of the magnetic fields in these young remnants. We suggest that N132D is older and probably somewhat more energetic and/or massive than Cas A. N103B appears to be a younger version of N132D, while 0519-690 is less luminous and not unlike the remnants of low-mass super-novae seen in the Milky Way.

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