Astronomy and Astrophysics – Astrophysics
Scientific paper
Apr 1994
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994pasau..11r..84m&link_type=abstract
Astronomical Society of Australia, Proceedings, vol. 11, no. 1, p. 84
Astronomy and Astrophysics
Astrophysics
Pulsars, Radio Sources (Astronomy), Stellar Evolution, Stellar Structure, Supernova Remnants, Astrophysics, Crab Nebula, Interstellar Matter, Radio Astronomy, Stellar Envelopes
Scientific paper
The morphology of supernova remnants is principally determined by two components, a shell formed by interaction of the supernova ejecta with the surrounding medium, and a nebula which is powered directly by the associated pulsar. This nebula, often called a 'plerion', is usually located within the shell. These two components appear to evolve independently; in many cases there is no detectable plerion and in a few cases, the Crab Nebula being the most notable example, there is no detectable shell. A 'theoretician's supernova remnant' has spherical symmetry, but observers know that this is rarely the case. There are four main possible sources of non-sphericity, namely, the surrounding interstellar medium, the circumstellar medium, the surpernova explosion, and the associated pulsar. Supernovae often occured in active star formation regions and these regions often have complex networks of cavities blown by strong stellar winds. A supernova remnant expanding in this environment can consist of a several shell-like structure. IC443 is a good example (Braun and Strom, 1986, Astron. Astrophys., 1264, 193). The enhancement of Supernova remnant (SNR) shell brightness toward the Galactic plane (Caswell, 1977, Proc. Astron. Soc. Aust., 3, 130) is further evidence of the influence of the large-scale structure of the interstellar medium. One of the most common forms of non-sphericity is a bilateral symmetry attributed to a barrel-shaped enhancement of the shell (Kesteven and Caswell, 1987, Astron. Astrophys., 183, 118). There is good evidence that this and the associated bi-annular structure often obseved (Manchester, 1987, Astron. Astrophys., 171, 205) ar due to structure in the circumstellar material resulting from mass loss from the pre-supernova star (Storey et al., 1992, Astron. Astrophys., 265, 752).
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