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Limitations of Stellar Abundance Determinations

Published online by Cambridge University Press:  19 July 2016

B. Baschek
B. Baschek*
Affiliation:
Institut für Theoretische Astrophysik Im Neuenheimer Feld 561 D-6900 Heidelberg Germany

Abstract

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The information content of (photospheric) stellar spectra and the accuracy of abundance determinations are discussed. Besides the physical properties of the line spectra, the spectral resolution, the signal-to-noise ratio, but also the incompleteness of the knowledge of the contributing blends limit the abundance information. For a perfect model atmosphere the main factors determining the accuracy of the abundances are S/N, the line saturation, and the location of the continuum (or, in a synthetic spectrum, the background of numerous lines). In addition systematic errors introduced by missing atomic data and an imperfect model atmosphere (non-LTE, line blanketing, hydrodynamics) are important. The typical accuracy of abundance determinations is discussed for main sequence stars for which the most reliable data are available, and for a few selected other stellar types.

Type
Setting the Stage
Information
Symposium - International Astronomical Union , Volume 145: Evolution of Stars: The Photospheric Abundance Connection , 1991 , pp. 39 - 47
Copyright
Copyright © Kluwer 1991 

References

Baschek, B.: 1984, Physica Scripta T8, 21 Google Scholar
Baschek, B.: 1990, Proc. Coll. on Atomic Spectra and Oscillator Strengths for Astrophysics and Fusion Research, Amsterdam 1989. Koninkl. Nederl. Akad. van Wetenschappen, in press Google Scholar
Baschek, B., Slettebak, A.: 1988, Astron. Astrophys. 207, 112 Google Scholar
Baschek, B., Heck, A., Jaschek, C., Jaschek, M., Köppen, J., Scholz, M., Wehrse, R.: 1984, Astron. Astrophys. 131, 378 Google Scholar
Bessell, M.S., Scholz, M.: 1990 in Accuracy of Element Abundances from Stellar Photospheres, Wehrse, R. (ed.), Lecture Notes in Physics 356, Springer, Heidelberg, p. 85 CrossRefGoogle Scholar
Butler, K.: 1990 in Accuracy of Element Abundances from Stellar Photospheres, Wehrse, R. (ed.), Lecture Notes in Physics 356, Springer, Heidelberg, p. 19 CrossRefGoogle Scholar
Cayrel, R.: 1988, in The Impact of Very High S/N Spectroscopy on Stellar Physics, IAU Symp. 132, Cayrel de Strobel, G., Spite, M. (eds.), Kluwer Academic Press, Dordrecht, p. 345 Google Scholar
Hansen, J.E., Ziegenbein, B., Lincke, R., Kelly, H.P.: 1977, J. Phys. B: Atom. Molec. Phys. 10, 37 Google Scholar
Hillier, D.J.: 1987, Astrophys. J. Suppl. Ser. 63, 965 CrossRefGoogle Scholar
Jaschek, M., Baschek, B., Jaschek, C., Heck, A.: 1985, Astron. Astrophys. 152, 439 Google Scholar
Jüttner, A., Reitermann, A., Stahl, O., Wolf, B.: 1989, Astron. Astrophys. Suppl. Ser. 81, 93 Google Scholar
Jüttner, A., Stahl, O., Wolf, B., Baschek, B.: 1990, in The Magellanic Clouds and Their Dynamical Interaction with the Milky Way, IAU Symp. 148, in press CrossRefGoogle Scholar
Kurucz, R.L.: 1981, Smithson. Astrophys. Obs. Spec. Report 390 Google Scholar
Kurucz, R.L.: 1990, Proc. Coll. on Atomic Spectra and Oscillator Strengths for Astrophysics and Fusion Research, Amsterdam 1989. Koninkl. Nederl. Akad. van Wetenschappen, in press Google Scholar
Landman, D.A., Roussel-Dupré, R. Tanigawa, G.: 1982, Astrophys. J. 261, 732 Google Scholar
Leinert, Ch., Haas, M., Allard, F., Wehrse, R., McCarthy, D.W. Jr., Jahreiss, H., Perrier, Ch.: 1990, Astron. Astrophys. 236, 399 Google Scholar
Mendez, R.H.: 1990 in Accuracy of Element Abundances from Stellar Photospheres, Wehrse, R. (ed.), Lecture Notes in Physics 356, Springer, Heidelberg, p. 45 Google Scholar
Mihalas, D.: 1990, in Astrophysics - Recent Progress and Future Possibilities, Gustafsson, B., Nissen, P.E. (eds.), Mat.-fys. Medd. 42:4, The Royal Danish Academy of Sciences and Letters, Copenhagen, p. 51 Google Scholar
Nugis, T.: 1982, in Wolf-Rayet Stars: Observations, Physics, Evolution, IAU Symp. 99, de Loore, C.W.H., Willis, A.J. (eds.), Reidel, Dordrecht, p. 131 CrossRefGoogle Scholar
Reitermann, A., Baschek, B., Stahl, O., Wolf, B.: 1990, Astron. Astrophys. 234, 109 Google Scholar
Sadakane, K.: 1990 in Accuracy of Element Abundances from Stellar Photospheres, Wehrse, R. (ed.), Lecture Notes in Physics 356, Springer, Heidelberg, p. 57 Google Scholar
Spite, F.: 1990 in Accuracy of Element Abundances from Stellar Photospheres, Wehrse, R. (ed.), Lecture Notes in Physics 356, Springer, Heidelberg, p. 69 Google Scholar
Venn, K., Lambert, D.L.: 1990, preprint Google Scholar
Wehrse, R. 1990, in Accuracy of Element Abundances from Stellar Photospheres, Wehrse, R. (ed.), Lecture Notes in Physics 356, Springer, Heidelberg, p. 1 Google Scholar
Wiese, W.L., Fuhr, J.R.: 1990, in Accuracy of Element Abundances from Stellar Photospheres, Wehrse, R. (ed.), Lecture Notes in Physics 356, Springer, Heidelberg, p. 7 Google Scholar
Willis, A.J.: 1982a, in Wolf-Rayet Stars: Observations, Physics, Evolution, IAU Symp. 99, de Loore, C.W.H., Willis, A.J. (eds.), Reidel, Dordrecht, p. 87 CrossRefGoogle Scholar
Willis, A.J.: 1982b, Mon. Not R. astr. Soc. 198, 897 Google Scholar