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The Oxygen Problem

Published online by Cambridge University Press:  30 March 2016

Michael S. Bessell
Michael S. Bessell*
Affiliation:
Mount Stromlo Observatory, Cotter Rd, ACT 2611, Australia

Abstract

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Permitted OI, forbidden [OI], electronic AΣ − XП UV OH and vib-rot IR OH lines often infer different oxygen abundances for cool stars. Which species should one use to determine the oxygen abundance in cool stars and how does one reconcile the different results for different species? Although there are uncertainties and systematic differences in the molecular gf values used by different authors, the main reason for the different results lies in the 1-D model atmosphere analyses that are used.

Type
II. Joint Discussions
Information
Highlights of Astronomy , Volume 12: Highlights of Astronomy. As presented at the XXIVth General Assembly of the IAU, 2000 , 2002 , pp. 410 - 412
Copyright
Copyright © Astronomical Society of Pacific 2002

References

Asplund, M. 2001, these proceedingsGoogle Scholar
Bessell, M.S. et al. 1998, A&A, 333, 231 Google Scholar
Boesgaard, A.M. et al. 1999, AJ, 117, 1549 Google Scholar
Castelli, F. 1999, A&A, 346, 564 Google Scholar
Fulbright, J.P. & Kraft, R.P. 1999, AJ, 118, 527 Google Scholar
Gillis, J.R. et al. 2000, JQSRT, in pressGoogle Scholar
Goldman, A. & Gillis, J.R. 1981, JQSRT, 25, 111 Google Scholar
Goldman, A. 2000 private communicationGoogle Scholar
Grevesse, N. & Sauval, A.J. 1999, A&A, 347, 348 Google Scholar
Israelian, G. et al. 1998, ApJ, 507, 8051 CrossRefGoogle Scholar
Kurucz, R.L. 1993, CDROM 15Google Scholar
Luque, J. & Crosley, D.R. 1998, JChPh, 109, 439 Google Scholar
Nissen, P. et al. 1994, A&A, 285, 440 Google Scholar