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Spectroscopic Abundance Determinations in M Supergiants

Published online by Cambridge University Press:  25 April 2016

P. J. McGregor
P. J. McGregor*
Affiliation:
Mount Stromlo and Siding Spring Observatories, Australian National University
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Extract

The M supergiants are rare objects in the solar neighbourhood and consequently until recently their importance has been largely overlooked. It is now being realized that these stars hold the key to extragalactic distance determinations since they can be detected at large distances while the maximum luminosity they attain seems to be remarkably constant and independent of galaxy type (Sandage and Tammann 1974; Humphreys 1978, 1979a, 1979b; Humphreys and Davidson 1979). They are also important in their own right since they are massive stars in the late stages of their evolution and undoubtedly suffer from mass loss and chemical enrichment due to the mixing of processed materials to their surfaces. In this light they can be considered as precursors of the luminous carbon stars and supernovae.

Type
Contributions
Information
Publications of the Astronomical Society of Australia , Volume 4 , Issue 1 , 1980 , pp. 93 - 95
Copyright
Copyright © Astronomical Society of Australia 1980

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References

Bell, R. A., Ericksson, K., Gustafsson, B., and Nördlund, Å., Astron. Astrophys. Suppl, 23, 37 (1976).Google Scholar
Fujita, Y., Interpretation of Spectra and Atmospheric Structure in Cool Stars, University of Tokyo Press (1970).Google Scholar
Griffin, R. R., A Photometric Atlas of the Spectrum of Arcturus, Cambridge Philosophical Society, (1968).Google Scholar
Humphreys, R. M., Astrophys. J. Suppl., 38, 309 (1978).Google Scholar
Humphreys, R. M., Astrophys. J., 234, 854 (1979a).Google Scholar
Humphreys, R. M., Astrophys. J., Suppl., 39, 389 (1979b).CrossRefGoogle Scholar
Humphreys, R. M., and Davidson, K., Astrophys. J., 232, 409 (1979).Google Scholar
Kurucz, R. L., Smithsonian Astrophys. Obs. Spec. Kept., No. 309 (1970).Google Scholar
Kurucz, R. L., and Peytremann, E., Smithsonian Astrophys. Obs. Spec. Rept., No. 362 (1975).Google Scholar
Sandage, A., and Tammann, G. A., Astrophys. J., 191, 603. (1974).CrossRefGoogle Scholar
White, N. M, and Wing, R. F., Astrophys. J., III, 209 (1978).CrossRefGoogle Scholar