Hostname: page-component-586b7cd67f-dlnhk Total loading time: 0 Render date: 2024-11-30T21:40:21.553Z Has data issue: false hasContentIssue false
  • English
  • Français

The [O/Fe] Ratio in Halo, Disk and Bulge Stars

Published online by Cambridge University Press:  07 August 2017

B. Barbuy
B. Barbuy*
Affiliation:
IAG-USP, Depto. Astronomia C.P. 9638, SÃo Paulo 01065, Brazil

Extract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

The oxygen-to-iron ratio in the different stellar populations is a tracer of the chemical enrichment by supernovae of types II and I: SNII/SNI along the Galaxy lifetime, given that the bulk of oxygen is produced and ejected by massive stars (M > 10 M⊙), whereas the bulk of iron is produced by SNI of intermediate masses. Otherwise, the O overabundances are generally accompanied by α-elements (24Mg, 28Si, 40Ca, 48Ti) overabundances (Wheeler et al, 1989).

Type
I. The Stellar Populations in the Milky Way
Information
Symposium - International Astronomical Union , Volume 149: The Stellar populations of Galaxies , 1992 , pp. 143 - 146
Copyright
Copyright © Kluwer 

References

Abia, C., Rebolo, R.: 1989, ApJ 347, 186.CrossRefGoogle Scholar
Barbuy, B.: 1983, A&A 123, 1.Google Scholar
Barbuy, B.: 1988, A&A 191, 121.Google Scholar
Barbuy, B., Erdelyi-Mendes, M.: 1989, A&A 214, 239.Google Scholar
Barbuy, B., Grenon, M.: 1991, A&A, to submit.Google Scholar
Barbuy, B., Castro, S., Ortolani, S., Bica, E.: 1991, A&A, submitted.Google Scholar
Bessell, M.S., Sutherland, R., Ruan, K.: 1991, preprint.Google Scholar
Brown, J.A., Wallerstein, G., Oke, J.B.: 1990, AJ 100, 1561.Google Scholar
Clegg, R.E.S., Lambert, D.L., Tomkin, J.: 1981, ApJ 250, 262.Google Scholar
Edvardsson, B., Gustafsson, B., Lambert, D.L., Nissen, P., Tomkin, J., Andersen, J.: 1991, preprint.Google Scholar
Gratton, R.: 1990, in IAU Symposium 145.Google Scholar
Gratton, R., Ortolani, S.: 1986, A&A 169, 201.Google Scholar
Kraft, R.P., Suntzeff, N.B., Langer, G.E., Carbon, D.F., Trefzger, C.F., Friel, E., Stone, R.P.S.: 1982, PASP 94, 55.Google Scholar
Kiselman, D.: 1991, A&A Letters 245, L9.Google Scholar
Lambert, D.L.: 1978, MNRAS 182, 279.Google Scholar
Lambert, D.L., Sneden, C., Ries, L.M.: 1974, ApJ 188, 97.Google Scholar
Leep, E.M., Wallerstein, G.: 1981, MNRAS 196, 543.Google Scholar
Luck, R.E., Bond, H.: 1985, ApJ 292, 559.CrossRefGoogle Scholar
Luck, R.E., Lambert, D.L.: 1985, ApJ 298, 782.Google Scholar
Nissen, P.E.: 1990, in Elements and the Cosmos , ed. Terlevich, R., Cambridge Univ. Press, in press.Google Scholar
Ortolani, S., Barbuy, B., Bica, E.: 1990, A&A 236, 362.Google Scholar
Pilachowski, C.A., Sneden, C., Wallerstein, G.: 1983, ApJS 52, 241.Google Scholar
Sneden, C., Lambert, D.L., Whitaker, R.W.: 1979, ApJ 234, 964.Google Scholar
Sneden, C., Kraft, R.P., Prosser, C.: 1990, in VI Cambridge Workshop on Cool Stars, Stellar Systems and the Sun , ed. Wallerstein, G., 369.Google Scholar
Spiesman, W.J., Wallerstein, G.: 1991, preprint.CrossRefGoogle Scholar
Spite, F., Spite, M.: 1978, A&A 67, 23.Google Scholar
Spite, F., Spite, M.: 1991, this symposium.Google Scholar
Tomkin, J., Lemke, M., Lambert, D., Sneden, C.: 1991, in preparation.Google Scholar
Wheeler, J.C., Sneden, C., Truran, J.W.: 1989, ARA&A 27, 279.Google Scholar