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The Effect of Non-LTE and Atmospheric Perturbations on Relative Abundance Determinations in Metal-Poor Giants

Published online by Cambridge University Press:  19 July 2016

Ruth C. Peterson
Ruth C. Peterson*
Affiliation:
Whipple Observatory, Smithsonian Institution, Steward Observatory, Room 458, University of Arizona, Tucson, AZ 85721

Abstract

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This paper reports an abundance analysis of spectra of 10 extremely metal-poor giants, including two in the globular cluster M92, in collaboration with Robert Kurucz and Eugene Avrett of the Center for Astrophysics and Bruce Carney of the University of North Carolina. An intercomparison of equivalent widths indicates that Luck and Bond have seriously overestimated the strengths of very weak lines and so deduced a spuriously high nickel abundance in the most metal-poor stars. A review of line-formation effects in the Sun strongly suggests that the rather high metallicities found for some extremely metal-poor stars by Pilachowski and coworkers is due to errors in their solar gf values, which unfortunately are unpublished. In our own analyses, stars with asymmetric H-alpha line profiles tend to have an excitation temperature at odds with the effective temperature found from infrared photometry. The discrepancy is removed by lowering the surface temperature by 100 K or by increasing the microturbulent velocity, either by a constant 0.5 km/s or by an amount which increases toward the surface. These changes have the most impact on those abundances deduced from strong lines or low-excitation lines of the neutral species; this includes sodium and barium as well as all the Fe I lines with very accurate gf values. Despite these difficulties, our findings reveal a low abundance for M92, and intrinsic scatter in the relationship between the relative abundances of sodium and oxygen and the overall iron abundance. In one field star, oxygen is apparently overabundant by an order of magnitude or more, while in the two M92 giants, the sodium abundance appears to differ by nearly this much.

Type
VI. Chemical Composition of Stars
Information
Symposium - International Astronomical Union , Volume 132: The Impact of Veryhigh S/N Spectroscopy on Stellar Physics , 1988 , pp. 493 - 499
Copyright
Copyright © Kluwer 1988 

References

Beckers, J. M., Bridges, C. A., and Gilliam, L B. 1976. A High Resolution Spectral Atlas of the Solar Irradiance From 380 to 700 Nanometers, AFGL-TR-76-0126.Google Scholar
Blackwell, D. E., Petford, A. D., and Simmons, G. J. 1982. M.N.R.A.S., 201, 595.CrossRefGoogle Scholar
Blackwell, D. E., and Shallis, M. J. 1979. M.N.R.A.S., 186, 673.Google Scholar
Buonanno, R., Corsi, C. E., and Fusi Pecci, F. 1985. Astron. Astrophys., 145, 97.Google Scholar
Cohen, J. G., Frogel, J. A., and Persson, S. E. 1978, Ap. J., 222, 165.Google Scholar
Delbouille, L., Roland, G., and Neven, L. 1973, Photometric Atlas of the Solar Spectrum from λ3000 to λ10000 (Liège: Institut d'Astrophysique).Google Scholar
Gustafsson, B., Bell, R. A., Eriksson, K., and Nordlund, A. 1975, Astron. Astrophys., 42, 407.Google Scholar
Holweger, H., and Müller, E. A. 1974, Solar Phys., 39, 19.Google Scholar
Kurucz, R. L. 1979, Ap. J. Suppl., 40, 1.Google Scholar
Luck, R. E., and Bond, H. E. 1985a, Ap. J., 292, 559.Google Scholar
Luck, R. E., and Bond, H. E. 1985b, Ap. J. Suppl., 49, 249.Google Scholar
Peterson, R. C., and Title, A. M. 1976, Appl. Opt. , 14, 2527.CrossRefGoogle Scholar
Pilachowski, C. A., Sneden, C., and Wallerstein, G. 1983. Ap. J. Suppl., 52, 541.CrossRefGoogle Scholar
Pilachowski, C. A., Wallerstein, G., and Leep, E. M. 1980, Ap. J., 236, 508.Google Scholar
Simmons, G. J., and Blackwell, D. E. 1982, Astron. Astrophys., 112, 209.Google Scholar
Sneden, C., and Parthasarathy, M. 1983. Ap. J., 267, 757.Google Scholar
Spite, M., and Spite, F. 1985, Ann. Rev. Astron. Astrophys., 23, 225.Google Scholar
Vernazza, J. E., Avrett, E. H., and Loeser, R. 1976, Ap. J. Suppl., 30, 1.Google Scholar