Hostname: page-component-76fb5796d-45l2p Total loading time: 0 Render date: 2024-04-26T22:59:47.926Z Has data issue: false hasContentIssue false
  • English
  • Français

Synthetic OH Band Spectra in G and K Stars

Published online by Cambridge University Press:  25 April 2016

M. S. Bessell ,
S. M. G. Hughes  and
P. L. Cottrell
M. S. Bessell
Affiliation:
Mount Stromio and Siding Spring Observatories, ANU.
S. M. G. Hughes
Affiliation:
Mount Stromio and Siding Spring Observatories, ANU.
P. L. Cottrell
Affiliation:
University of Canterbury N.Z.
Get access Rights & Permissions [Opens in a new window]

Extract

Carbon, nitrogen and oxygen are of interest for stellar and galactic evolution for four main reasons. Firstly, they comprise most of the mass of elements heavier than helium, so their abundance reflects the bulk of chemical enrichment. Secondly, all of the oxygen, much of the carbon and perhaps some of the nitrogen is believed to be produced in shorter-lived stars more massive than those responsible for the Fe production (Tinsley 1979), so their abundance relative to Fe in very metal deficient objects should provide key information for modelling the chemical history of galaxies. Thirdly, because C and O comprise the bulk of the metals in stellar material (Fe:C:N:0 = 1:12:2.5:21 in the Sun) it is their abundance as well as that of iron, which is needed to compute evolutionary tracks for different metallicities. Finally, the O abundance will indicate whether CNO material has been mixed to the surface.

Type
Contributions
Information
Publications of the Astronomical Society of Australia , Volume 5 , Issue 4 , 1984 , pp. 547 - 552
Copyright
Copyright © Astronomical Society of Australia 1984

Access options

Get access to the full version of this content by using one of the access options below. (Log in options will check for institutional or personal access. Content may require purchase if you do not have access.)

References

Bell, R. A., Eriksson, K., Gustafsson, B., and Nördlund, Å. Astron Astrophys Suppl., 23, 37 (1971).Google Scholar
Bessell, M. S. and Norris, J., Astrophys. J. (Lett.), 263, L29 (1982).Google Scholar
Bidelman, W. P. and MacConnell, D. J., Astron. J., 78, 687 (1973).Google Scholar
Conti, P. S., Greenstein, J. L., Spinrad, H., Wallerstein, G. and Vardya, M. S., Astrophys J., 148, 105 (1967).Google Scholar
Cottrell, P. L., PhD Thesis, ANU (1978)Google Scholar
Cottrell, P. L. and Norris, J., Astrophys J. 221, 893 (1978).Google Scholar
Goldman, A., and Gillis, J. R., J. Quant, Spectrosc. Radiat. Transfer, 25, 111 (1981).Google Scholar
Kurucz, R. L., SAO Spec. Rept., No. 309 (1970).Google Scholar
Lambert, D. L., Mon. Not. R. Astron. Soc., 182, 249 (1978).Google Scholar
Lambert, D. L., Sneden, C., and Ries, L. M., Astrophys. J., 188, (1974).Google Scholar
Moore, C. E., Minnaert, M. G. J. and Houtgast, J., NBS Monograph No. 61 (1966).Google Scholar
Norris, J., Bessell, M. S. and Pickles, A. J., in preparation (1984).Google Scholar
Sneden, C. 1973, Astrophys. J., 184, 839 (1973).Google Scholar
Tinsley, B. M., Astrophys J., 229, 1046 (1979).Google Scholar
Wehrse, R., private communication (1979).Google Scholar