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Two remarkable bright supernova remnants

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Abstract

Statistical studies of supernova remnants (SNRs) indicate that the objects of high surface brightness are young1. This is confirmed by measurements of angular expansion for a number of such remnants and by the secular decrease in their radio flux densities2. Studies of these young SNRs are of particular interest as they can impose constraints on models of supernova outbursts and can reveal details of the initial interaction between the rapidly-expanding stellar material and the ambient interstellar medium3. Also, a high percentage of bright remnants belong to the comparatively-rare class of filled-centre SNRs. However, because of their small angular sizes, many have not been observed with sufficient resolution to determine detailed structures or, in some cases, even to verify an SNR classification. Between July 1981 and August 1984, we used the Very Large Array (VLA) of the National Radio Astronomy Observatory (NRAO) in its B, C and D configurations to clarify the morphology of several high-brightness sources from the Milne SNR catalogue4. Of these, the two sources G349.7+0.2 and G357.7−0.1 were found to be most unusual.

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Authors and Affiliations

  1. European Southern Observatory, Karl-Schwarzschild-Strasse 2, D-8046, Garching bei München, FRG

    P. A. Shaver

  2. National Radio Astronomy Observatory, 949 North Cherry Avenue, Campus Building 65, Tucson, Arizona, 85721-0655, USA

    C. J. Salter

  3. Tata Institute of Fundamental Research Centre, Indian Institute of Science Campus, PO Box 1234, Bangalore, 560 012, India

    C. J. Salter & A. R. Patnaik

  4. National Radio Astronomy Observatory, PO Box 0, Socorro, New Mexico, 87801, USA

    J. H. van Gorkom & G. C. Hunt

Authors
  1. P. A. Shaver
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  2. C. J. Salter
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  3. A. R. Patnaik
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  4. J. H. van Gorkom
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  5. G. C. Hunt
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Shaver, P., Salter, C., Patnaik, A. et al. Two remarkable bright supernova remnants. Nature 313, 113–115 (1985). https://doi.org/10.1038/313113a0

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  • DOI: https://doi.org/10.1038/313113a0

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