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CNO and F abundances in the barium star HD 123396
| Indexado |
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| DOI | 10.1051/0004-6361/201116604 | ||||
| Año | 2011 | ||||
| Tipo | artículo de investigación |
Citas Totales
Autores Afiliación Chile
Instituciones Chile
% Participación
Internacional
Autores
Afiliación Extranjera
Instituciones
Extranjeras
Abstract
Conclusions. The observed abundance pattern of the light elements (CNO, F, and Na) recovered here as well as the heavy elements (s-process) studied elsewhere suggest that the surface composition of HD 123396 is well fitted by the predicted abundance pattern of a 1.5 M-circle dot AGB model star with Z = 0.001. Thus, the AGB mass transfer hypothesis offers a quantitatively viable framework.
| Ord. | Autor | Género | Institución - País |
|---|---|---|---|
| 1 | ALVES-BRITO, ALAN | Hombre |
Pontificia Universidad Católica de Chile - Chile
Swinburne Univ Technol - Australia Swinburne University of Technology - Australia |
| 2 | Karakas, A. | Mujer |
Australian Natl Univ - Australia
Australian National University - Australia The Australian National University - Australia |
| 3 | Yong, D. | Hombre |
Australian Natl Univ - Australia
Australian National University - Australia The Australian National University - Australia |
| 4 | Melendez, J. | Hombre |
UNIV SAO PAULO - Brasil
Universidade de Sao Paulo - USP - Brasil Universidade de São Paulo - Brasil |
| 5 | VASQUEZ-ARANCIBIA, SERGIO OCTAVIO | Hombre |
Pontificia Universidad Católica de Chile - Chile
|
| Fuente |
|---|
| FONDECYT |
| National Science Foundation |
| CNPq |
| FAPESP |
| Conselho Nacional de Desenvolvimento Científico e Tecnológico |
| CONICYT (Chile) |
| Fondo Nacional de Desarrollo Científico y Tecnológico |
| Fundação de Amparo à Pesquisa do Estado de São Paulo |
| Comisión Nacional de Investigación Científica y Tecnológica |
| Australian Research Council |
| NSF |
| Ministerio de Ciencia, Tecnología e Innovación Productiva |
| National Research Council |
| Comisión Nacional de Investigación CientÃfica y Tecnológica |
| Fundação de Amparo à Pesquisa do Estado de São Paulo |
| Science and Technology Facilities Council |
| Fondo Nacional de Desarrollo CientÃfico y Tecnológico |
| Conselho Nacional de Desenvolvimento CientÃfico e Tecnológico |
| Ministerio da Ciencia e Tecnologia |
| Ministerio da Ciencia e Tecnologia (Brazil) |
| Ministerio de Ciencia, TecnologÃa e Innovación Productiva |
| Australian Research Council (Australia) |
| National Research Council (Canada) |
| National Science Foundation (United States) |
| Ministério da Ciência e Tecnologia |
| Science and Technology Facilities Council (United Kingdom) |
| USP (Novos Docentes) |
| CNPq (Bolsa de Produtividade) |
| Ministerio de Ciencia, Tecnologia a e Innovacion Productiva (Argentina) |
| Australian Gemini Office |
| Agradecimiento |
|---|
| A.A.B. acknowledges CNPq (PDE, 200227/2008-4) and FONDECYT (3100013) for financial support and Dr. S. Ryder, from the Australian Gemini Office, for his assistance during the Phase II definitions of our Gemini/Phoenix observations. J.M. acknowledges support from FAPESP (2010/50930-6), USP (Novos Docentes), and CNPq (Bolsa de produtividade). We are grateful to Drs. D. Allen and R. Gallino for kindly answering our questions on their results and to Dr. M. Lugaro for help in preparing the nuclear network used in the nucleosynthesis code. We are also grateful to an anonymous referee for detailed and useful comments on a previous version of the paper. The spectra were obtained as part of the programme GS-2009A-Q-26. Based on observations obtained at the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the Science and Technology Facilities Council (United Kingdom), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), Ministerio da Ciencia e Tecnologia (Brazil), and Ministerio de Ciencia, Tecnologia a e Innovacion Productiva (Argentina). |
| A.A.B. acknowledges CNPq (PDE, 200227/2008-4) and FONDECYT (3100013) for financial support and Dr. S. Ryder, from the Australian Gemini Office, for his assistance during the Phase II definitions of our Gemini/Phoenix observations. J.M. acknowledges support from FAPESP (2010/50930-6), USP (Novos Docentes), and CNPq (Bolsa de produtividade). We are grateful to Drs. D. Allen and R. Gallino for kindly answering our questions on their results and to Dr. M. Lugaro for help in preparing the nuclear network used in the nucleosynthesis code. We are also grateful to an anonymous referee for detailed and useful comments on a previous version of the paper. The spectra were obtained as part of the programme GS-2009A-Q-26. Based on observations obtained at the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the Science and Technology Facilities Council (United Kingdom), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), Ministério da Ciência e Tecnologia (Brazil), and Ministerio de Ciencia, Tecnología e Innovación Productiva (Argentina). |
