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Photometry and Spectroscopy of Long Period Variables in the Magellanic Clouds

Published online by Cambridge University Press:  25 April 2016

P. R. Wood ,
M. S. Bessell  and
M. W. Fox
P. R. Wood
Affiliation:
Mt Stromlo and Siding Spring Observatories, The Australian National University
M. S. Bessell
Affiliation:
Mt Stromlo and Siding Spring Observatories, The Australian National University
M. W. Fox
Affiliation:
Mt Stromlo and Siding Spring Observatories, The Australian National University
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Extract

Many of the important events in the life of a star occur, or are thought to occur, during the red giant or supergiant phase of evolution. For example, in heavy and intermediate mass stars supernova explosions terminate normal evolutionary processes while in lower mass stars the stellar envelope is entirely removed giving rise to planetary nebulae and, subsequently, white dwarfs. Theoretical calculations suggest that before the onset of these rather drastic events, a significant amount of nucleosynthesis occurs, giving rise to enhanced surface abundances of He, C, N and s-process elements (e.g., Iben and Truran 1978; Renzini and Voli 1981); loss of the envelope material by stellar winds, planetary nebula ejection and supernova explosions produce overall galactic enrichment in these elements.

Type
Contributions
Information
Publications of the Astronomical Society of Australia , Volume 4 , Issue 2 , 1981 , pp. 203 - 205
Copyright
Copyright © Astronomical Society of Australia 1981

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References

Edmunds, M. G. and Pagel, B. E. J. Mon. Not. R. Astron. Soc., 185, 77p (1978).Google Scholar
Feast, M. W., Catchpole, R. M., Carter, B. S. and Roberts, G. Mon. Not. R. Astron. Soc., 193, 377 (1980).Google Scholar
Frogel, J. A. Persson, S. E. and Cohen, J. G. Astrophys J., 239, 495 (1980).Google Scholar
Glass, I. S. Mon. Not. R. Astron. Soc., 186, 317 (1979).Google Scholar
Glass, I. S. and Lloyd Evans, T. Nature, in press (1981).Google Scholar
Iben, I. Astrophys. J., 196, 525 (1975). Iben, I. Astrophys. J., 217, 788 (1977).Google Scholar
Iben, I. and Truran, J. W. Astrophys. J., 220, 980 (1978).Google Scholar
Lamb, S. A., Iben, I. and Howard, W. M. Astrophys. J., 207, 209 (1976).Google Scholar
Paczynski, B. Astrophys. J., 214, 812 (1977).Google Scholar
Renzini, A. and Voli, M. Astron. Astrophys., 94, 175 (1981).Google Scholar
Ridgway, S. T., Joyce, R. R., White, N. M. and Wing, R. F. Astrophys. J., 235, 126 (1980).Google Scholar
Robertson, B. S. C. and Feast, M. W. Mon. Not. R. Astron. Soc., in press (1981).Google Scholar
Wood, P. R., in I.A.U. Colloquium 46, “ Changing trends in variable star research ”, eds. Bateson, F. M., Smak, J. and Urch, I. M., p. 163 (1978).Google Scholar
Wood, P. R., in ‘ Physicalprocesses in red giants ’, eds. Iben, I. and Renzini, A. (Reidel) (1980).Google Scholar