Hostname: page-component-78c5997874-xbtfd Total loading time: 0 Render date: 2024-11-08T02:53:11.916Z Has data issue: false hasContentIssue false
  • English
  • Français

Abundances of the elements in the halo stars, interaction between observation and theory

Published online by Cambridge University Press:  25 May 2016

M. Spite
M. Spite*
Affiliation:
Observatoire de Paris-Meudon F-92195 Meudon principal Cedex, FRANCE

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 halo stars are very old stars formed at the beginning of the evolution of the Galaxy. Their main characteristic is that their atmosphere is very metal-poor since at the time of their birth, the matter of the Galaxy had been enriched by only a few number of supernovae. The first very metal deficient stars have been studied in the sixties: Baschek (1959), Aller and Greenstein(1960) Wallerstein et al. (1963). The stellar models used in these first studies were rather crude: the atmosphere of the stars was represented by only one layer with a mean temperature and a mean electronic pressure, the continuum opacity was supposed to be due to H− and included in addition only the contribution by Rayleigh scattering. Later rescaled solar models were used and finally, at the end of the seventies, grids of theoretical models more and more sophisticated became available.

Type
Stellar Abundances
Information
Symposium - International Astronomical Union , Volume 189: Fundamental Stellar Properties: The Interaction Between Observation and Theory , 1997 , pp. 185 - 192
Copyright
Copyright © Kluwer 1997 

References

Aller, L.H., Greenstein, J.L. (1960) ApJS 5, 139 Google Scholar
Balachandran, S., Carney, B.W. (1996) AJ 111, 946 CrossRefGoogle Scholar
Barbuy, B., Erdelyi-Mendes, M. (1989) A&A 214, 239 Google Scholar
Baschek, B. (1959) Zs. f. Ap 48, 95 Google Scholar
Bessell, M.S., Sutherland, R.S., Ruan, K. (1991) ApJ 383, L71 Google Scholar
Bonifacio, P., Molaro, P. (1997) MNRAS in press Google Scholar
Cavallo, R.M., Pilachowski, C.A., Rebolo, R. (1997) PASP submittedGoogle Scholar
Cayrel de Strobel, G., Soubiran, C., Friel, E.B., Ralite, N., François, (1997) A&AS in press Google Scholar
Cayrel, R., (1988) in IAU Symp 132 “The impact of Very High S/N Spectroscopy on Stellar Physics”, Cayrel de Strobel, G. and Spite, M. eds., Kluwer, p.345 Google Scholar
Charbonnel, C., Vauclair, S. (1995) A&A 295, 715 Google Scholar
Edvardsson, B., Anderssen, J., Gustafsson, B., Lambert, D.L., Nissen, P.E., Tomkin, J. (1993) A&A 275, 101 Google Scholar
Gustafsson, B., Bell, R.A., Eriksson, K., Nordlund, Å (1975) A&A 42, 407 Google Scholar
Gratton, R., Ortolani, S. (1986), A&A 169, 201 Google Scholar
King, J.R. (1993) A J 106, 1206 CrossRefGoogle Scholar
Kiselman, D. (1991) A&A 245, L9 Google Scholar
Molaro, P., Primas, F., Bonifacio, P. (1995), A&A 295, L47 Google Scholar
Nissen, P.E., Edvardsson, B. (1992) A&A 261, 255 Google Scholar
Nissen, P.E., Gustafsson, B., Edvardsson, B., Gilmore, G. (1994) A&A 285, 440 Google Scholar
Norris, J. E., Ryan, S. G., Stringfellow, G. S. (1994) ApJ 423, 386 Google Scholar
Pinsonneault, M.H., Deliyannis, C.P., Demarque, P. (1992) ApJS 78, 179 Google Scholar
Ryan, S.G., Beers, T.C., Deliyannis, C., Thorburn, J.A. (1996) ApJ 458, 543 Google Scholar
Shetrone, M.D. (1996) AJ 112, 1517 CrossRefGoogle Scholar
Sneden, C., Kraft, R.P., Prosser, C.F., Langer, G.E. (1991) AJ 102, 2001 Google Scholar
Spite, M., Spite, F.: (1991) A&A 252, 689 Google Scholar
Spite, M., François, P., Nissen, P.E., Spite, F. (1996) A&A 307, 172 Google Scholar
Tomkin, J., Lemke, M., Lambert, D.L., Sneden, C. (1992) AJ 104, 1568 Google Scholar
Thorburn, J.A., (1994) ApJ 421, 318 CrossRefGoogle Scholar
Wallerstein, G., Greenstein, J.L., Parker, R., Heifer, H.L., Aller, L.H. (1963) ApJ 137, 280 Google Scholar