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Abundances of the heavy elements in the Magellanic Clouds. III - Interpretation of results
Russell, Stephen C.; Dopita, Michael A.
AA(Dublin Institute for Advanced Studies, Republic of Ireland), AB(Mount Stromlo and Siding Spring Observatoires, Canberra, Australia)
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 384, Jan. 10, 1992, p. 508-522. (ApJ Homepage)
Publication Date:
NASA/STI Keywords:
Abundance, Interstellar Matter, Magellanic Clouds, Milky Way Galaxy, Nuclear Fusion, Star Formation, Chemical Evolution, Galactic Evolution, Heavy Elements, Nuclear Reactions
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The observed chemical abundances of the Magellanic Clouds are interpreted in terms of the star formation histories of the Clouds and the relationships between the chemical evolutionary histories of each of the Clouds and with the solar evolution in the Galaxy. It is found that the interstellar medium (ISM) of the LMC has a mean metallicity 0.2 dex lower than the local ISM, and the metallicity of the SMC is 0.6 dex lower. However, the interstellar media of both the Magellanic Clouds and the Galaxy have significantly nonsolar elemental ratios. It is also shown that the stellar carbon abundances in the clouds appear normal, and therefore it is the H II regions that must be overdefficient in this element.

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