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Carbon and Nitrogen in Halo Stars

Published online by Cambridge University Press:  12 April 2016

Christopher Sneden  and
Ruth C. Peterson
Christopher Sneden
Affiliation:
University of Wyoming
Ruth C. Peterson
Affiliation:
Lockheed Solar Observatory

Abstract

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A new study of carbon and nitrogen abundances has been carried out for a sample of halo dwarf stars. This sample was limited to relatively bright high velocity stars with substantial metal deficiencies (-0.65≥[Fe/H]≥ −2.00). Synthesis of CH molecular bands for nine program stars indicates that [c/Fe] = −0.1±0.2 in halo stars. Preliminary results of the NH synthesis in two stars shows discrepant results: a moderate velocity star has [N/Fe]≲ −1.0 while a very high velocity star has [N/Fe]⋍ +0.0. Implications of these abundances for galactic chemical evolution are discussed.

Type
Part III: The Chemical Properties of the Disc and the Halo in our Galaxy
Information
International Astronomical Union Colloquium , Volume 45: Chemical and Dynamical Evolution of our Galaxy , September 1977 , pp. 201 - 204
Copyright
Copyright © Geneva Observatory 1977

References

Audouze, J., Lequeux, J., and Vigroux, L. 1975, Astron. Astrophys. 43, 71.Google Scholar
Bell, R. A. 1970, Monthly Notices Roy. Astron. Soc, 148, 25.Google Scholar
Clegg, R. E. S. 1975, Thesis, University of Maryland.Google Scholar
Pagel, B. E. J. 1971, Memoirs Roy. Astron. Soc, 11, 172.Google Scholar
Peterson, R. C. 1977, submitted to Astrophys. J.Google Scholar
Peterson, R. C. and Sneden, C. 1978, to be published.Google Scholar
Torres-Peimbert, S. and Pelmbert, M. 1977, preprint.Google Scholar