The Rise of the s-Process in the Galaxy
(2004) In The Astrophysical Journal 617(2). p.1091-1114- Abstract
- From newly obtained high-resolution, high signal-to-noise ratio spectra the abundances of the elements La and Eu have been determined over the stellar metallicity range -3<[Fe/H]<+0.3 in 159 giant and dwarf stars. Lanthanum is predominantly made by the s-process in the solar system, while Eu owes most of its solar system abundance to the r-process. The changing ratio of these elements in stars over a wide metallicity range traces the changing contributions of these two processes to the Galactic abundance mix. Large s-process abundances can be the result of mass transfer from very evolved stars, so to identify these cases we also report carbon abundances in our metal-poor stars. Results indicate that the s-process may be active as... (More)
- From newly obtained high-resolution, high signal-to-noise ratio spectra the abundances of the elements La and Eu have been determined over the stellar metallicity range -3<[Fe/H]<+0.3 in 159 giant and dwarf stars. Lanthanum is predominantly made by the s-process in the solar system, while Eu owes most of its solar system abundance to the r-process. The changing ratio of these elements in stars over a wide metallicity range traces the changing contributions of these two processes to the Galactic abundance mix. Large s-process abundances can be the result of mass transfer from very evolved stars, so to identify these cases we also report carbon abundances in our metal-poor stars. Results indicate that the s-process may be active as early as [Fe/H]=-2.6, although we also find that some stars as metal-rich as [Fe/H]=-1 show no strong indication of s-process enrichment. There is a significant spread in the level of s-process enrichment even at solar metallicity. (Less)
Please use this url to cite or link to this publication:
https://lup.lub.lu.se/record/964926
- author
- Simmerer, Jennifer LU ; Sneden, Christopher ; Cowan, John ; Collier, Jason ; Woolf, Vincent and Lawler, James
- organization
- publishing date
- 2004
- type
- Contribution to journal
- publication status
- published
- subject
- in
- The Astrophysical Journal
- volume
- 617
- issue
- 2
- pages
- 1091 - 1114
- publisher
- American Astronomical Society
- external identifiers
-
- scopus:13944273470
- language
- English
- LU publication?
- no
- id
- 3033da09-88ca-48c9-9c82-557e43e24a63 (old id 964926)
- date added to LUP
- 2016-04-04 13:52:39
- date last changed
- 2022-04-24 03:42:53
@article{3033da09-88ca-48c9-9c82-557e43e24a63, abstract = {{From newly obtained high-resolution, high signal-to-noise ratio spectra the abundances of the elements La and Eu have been determined over the stellar metallicity range -3<[Fe/H]<+0.3 in 159 giant and dwarf stars. Lanthanum is predominantly made by the s-process in the solar system, while Eu owes most of its solar system abundance to the r-process. The changing ratio of these elements in stars over a wide metallicity range traces the changing contributions of these two processes to the Galactic abundance mix. Large s-process abundances can be the result of mass transfer from very evolved stars, so to identify these cases we also report carbon abundances in our metal-poor stars. Results indicate that the s-process may be active as early as [Fe/H]=-2.6, although we also find that some stars as metal-rich as [Fe/H]=-1 show no strong indication of s-process enrichment. There is a significant spread in the level of s-process enrichment even at solar metallicity.}}, author = {{Simmerer, Jennifer and Sneden, Christopher and Cowan, John and Collier, Jason and Woolf, Vincent and Lawler, James}}, language = {{eng}}, number = {{2}}, pages = {{1091--1114}}, publisher = {{American Astronomical Society}}, series = {{The Astrophysical Journal}}, title = {{The Rise of the s-Process in the Galaxy}}, volume = {{617}}, year = {{2004}}, }