Hostname: page-component-7c8c6479df-fqc5m Total loading time: 0 Render date: 2024-03-27T01:53:36.707Z Has data issue: false hasContentIssue false

The evolution of C and O abundances in stellar populations

Published online by Cambridge University Press:  06 January 2014

Poul E. Nissen
Affiliation:
Stellar Astrophysics Centre, Dept. of Physics and Astronomy, Aarhus University, Denmark email: pen@phys.au.dk
William J. Schuster
Affiliation:
Observatorio Astronomico National, UNAM, Ensenada, B.C.Mexico email: schuster@astrosen.unam.mx
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

Carbon and oxygen abundances in F and G main-sequence stars ranging in metallicity from [Fe/H] = −1.6 to +0.5 are determined from a non-LTE analysis of C i and O i atomic lines in high-resolution spectra. Both C and O are good tracers of stellar populations; distinct trends of [C/Fe] and [O/Fe] as a function of [Fe/H] are found for high- and low-alpha halo stars and for thick- and thin-disk stars. These trends and that of [C/O] provide new information on the nucleosynthesis sites of carbon and the time-scale for the chemical enrichment of the various Galactic components.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2014 

References

Adibekyan, V. Zh., Sousa, S. G., Santos, N. C., et al. 2012, A&A, 545, A32Google Scholar
Bensby, T. & Feltzing, S. 2006, MNRAS, 367, 1181Google Scholar
Casagrande, L., Ramírez, I., Meléndez, J., Bessell, M., & Asplund, M. 2010, A&A, 512, A54Google Scholar
Fabbian, D., Asplund, M., Barklem, P. S., Carlsson, M., & Kiselman, D. 2009a, A&A, 500, 1221Google Scholar
Fabbian, D., Nissen, P. E., Asplund, M., Pettini, M., Akerman, C. 2009b, A&A, 500, 1143Google Scholar
Font, A. S., McCarthy, I. G., Crain, R. A., et al. 2011, MNRAS, 416, 2802Google Scholar
Gustafsson, B., Edvardsson, B., Eriksson, K., et al. 2008, A&A, 486, 951Google Scholar
Kobayashi, C., Karakas, A. I., & Umeda, H. 2011, MNRAS, 414, 3231CrossRefGoogle Scholar
McCarthy, I. G., Font, A. S., Crain, R. A., et al. 2012, MNRAS, 420, 2245Google Scholar
Nissen, P. E. 2013, A&A, 552, A73Google Scholar
Nissen, P. E. & Schuster, W. J. 2010, A&A 511 L10 (NS10)Google Scholar
Nissen, P. E. & Schuster, W. J. 2011, A&A, 530, A15Google Scholar
Ramírez, I., Meléndez, J., & Chanamé, J. 2012, ApJ, 757, 164Google Scholar
Schuster, W. J., Moreno, E., Nissen, P. E., & Pichardo, B. 2012, A&A, 538, A21Google Scholar
Takeda, Y. & Honda, S. 2005, PASJ, 57, 65Google Scholar
Zolotov, A., Willman, B., Brooks, A. M., et al. 2010, ApJ, 721, 738Google Scholar