Optical observations of SNRs in the Magellanic Clouds

Details Optical observations of SNRs in the Magellanic Clouds Optical observations of SNRs in the Magellanic Clouds

Mar 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979aujph..32..123d&link_type=abstract

(Joint Australia-USSR-USA Symposium on Pulsars and Supernova Remnants, Sydney, Australia, Apr. 1978.) Australian Journal of Phys

Physics

1

Magellanic Clouds, Supernova Remnants, Visual Observation, Abundance, Nickel, Oxygen Ions, Radial Velocity, Shock Waves

Scientific paper

The standard picture of supernova-remnant (SNR) evolution is discussed, along with implications of optical and X-ray observations of SNRs in the Galaxy. The case of Magellanic Cloud SNRs is then considered in detail. The technique used for optical identification of SNRs in the Magellanic Clouds is described, and physical conditions in SNR shocks are analyzed on the basis of optical studies of Magellanic Cloud SNRs. Some qualitative results on abundances in the Magellanic Cloud SNRs are examined and compared with similar data for Galactic SNRs, particularly with respect to nitrogen. It is concluded that a model of shocks moving into dense clouds embedded in a medium of lower density, whose initial density varies approximately as the inverse square of distance, seems to be the only reasonably simple model that can explain the observations of Magellanic Cloud SNRs.

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