The s-process at low metallicity

Richard J. Stancliffe; Maria A. Lugaro; Amanda I. Karakas; Carlos Rijs

doi:10.1063/1.4754347

The s-process at low metallicity

Richard J. Stancliffe, Maria A. Lugaro, Amanda I. Karakas, Carlos Rijs

Research output: Chapter in Book/Report/Conference proceeding › Conference Paper › Research

1 Citation (Scopus)

Abstract

We present models for the slow neutron-capture process (s-process) in asymptotic giant branch stars of metallicity [Fe/H] = -2.3 and masses 0.9 - 6M_⊙. The models where the 13C burns radiatively (stars of around 2M_⊙) produce an overall good match to carbon-enhanced metalpoor (CEMP) stars showing barium enhancements (CEMP-s). On the other hand, none of our models can provide a match to the composition of CEMP stars showing both barium and europium enhancements (CEMP-s/r). The models fail to reproduce the observed Eu abundances, and they also fail to reproduce the correlation between the Eu and Ba abundances. They also cannot match the ratio of heavy-to-light s-process elements observed in many CEMP-s/r stars, which can be more than 10 times higher than in the Solar System. This work has been published [1] and the interested reader should refer to that work for further details, included published tables of yields.

Original language	English
Title of host publication	First Stars IV - From Hayashi to the Future
Subtitle of host publication	Kyoto, Japan; 21-25 May 2012
Editors	Masayuki Umemura, Kazuyuki Omukai
Place of Publication	USA
Publisher	AIP Publishing
Pages	156-159
Number of pages	4
ISBN (Print)	9780735410923
DOIs	https://doi.org/10.1063/1.4754347
Publication status	Published - 2012
Event	Conference on FIRST STARS - From Hayashi to the Future 2012 - Kyoto, Japan Duration: 21 May 2012 → 25 May 2012 Conference number: 4th

Publication series

Name	AIP Conference Proceedings
Publisher	AIP Publishing
Volume	1480
ISSN (Print)	0094-243x

Conference

Conference	Conference on FIRST STARS - From Hayashi to the Future 2012
Country/Territory	Japan
City	Kyoto
Period	21/05/12 → 25/05/12

Keywords

abundances
nuclear reactions
nucleosynthesis
stars: abundances
stars: AGB and post-AGB

Access to Document

10.1063/1.4754347

Cite this

@inproceedings{793c8478920d4e88b34556dff7dd6b23,

title = "The s-process at low metallicity",

abstract = "We present models for the slow neutron-capture process (s-process) in asymptotic giant branch stars of metallicity [Fe/H] = -2.3 and masses 0.9 - 6M⊙. The models where the 13C burns radiatively (stars of around 2M⊙) produce an overall good match to carbon-enhanced metalpoor (CEMP) stars showing barium enhancements (CEMP-s). On the other hand, none of our models can provide a match to the composition of CEMP stars showing both barium and europium enhancements (CEMP-s/r). The models fail to reproduce the observed Eu abundances, and they also fail to reproduce the correlation between the Eu and Ba abundances. They also cannot match the ratio of heavy-to-light s-process elements observed in many CEMP-s/r stars, which can be more than 10 times higher than in the Solar System. This work has been published [1] and the interested reader should refer to that work for further details, included published tables of yields.",

keywords = "abundances, nuclear reactions, nucleosynthesis, stars: abundances, stars: AGB and post-AGB",

author = "Stancliffe, {Richard J.} and Lugaro, {Maria A.} and Karakas, {Amanda I.} and Carlos Rijs",

year = "2012",

doi = "10.1063/1.4754347",

language = "English",

isbn = "9780735410923",

series = "AIP Conference Proceedings",

publisher = "AIP Publishing",

pages = "156--159",

editor = "Masayuki Umemura and Kazuyuki Omukai",

booktitle = "First Stars IV - From Hayashi to the Future",

address = "United States of America",

note = "Conference on FIRST STARS - From Hayashi to the Future 2012 ; Conference date: 21-05-2012 Through 25-05-2012",

}

Stancliffe, RJ, Lugaro, MA, Karakas, AI & Rijs, C 2012, The s-process at low metallicity. in M Umemura & K Omukai (eds), First Stars IV - From Hayashi to the Future: Kyoto, Japan; 21-25 May 2012. AIP Conference Proceedings, vol. 1480, AIP Publishing, USA, pp. 156-159, Conference on FIRST STARS - From Hayashi to the Future 2012, Kyoto, Japan, 21/05/12. https://doi.org/10.1063/1.4754347

The s-process at low metallicity. / Stancliffe, Richard J.; Lugaro, Maria A.; Karakas, Amanda I. et al.

First Stars IV - From Hayashi to the Future: Kyoto, Japan; 21-25 May 2012. ed. / Masayuki Umemura; Kazuyuki Omukai. USA : AIP Publishing, 2012. p. 156-159 (AIP Conference Proceedings; Vol. 1480).

Research output: Chapter in Book/Report/Conference proceeding › Conference Paper › Research

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T1 - The s-process at low metallicity

AU - Stancliffe, Richard J.

AU - Lugaro, Maria A.

AU - Karakas, Amanda I.

AU - Rijs, Carlos

N1 - Conference code: 4th

PY - 2012

Y1 - 2012

N2 - We present models for the slow neutron-capture process (s-process) in asymptotic giant branch stars of metallicity [Fe/H] = -2.3 and masses 0.9 - 6M⊙. The models where the 13C burns radiatively (stars of around 2M⊙) produce an overall good match to carbon-enhanced metalpoor (CEMP) stars showing barium enhancements (CEMP-s). On the other hand, none of our models can provide a match to the composition of CEMP stars showing both barium and europium enhancements (CEMP-s/r). The models fail to reproduce the observed Eu abundances, and they also fail to reproduce the correlation between the Eu and Ba abundances. They also cannot match the ratio of heavy-to-light s-process elements observed in many CEMP-s/r stars, which can be more than 10 times higher than in the Solar System. This work has been published [1] and the interested reader should refer to that work for further details, included published tables of yields.

AB - We present models for the slow neutron-capture process (s-process) in asymptotic giant branch stars of metallicity [Fe/H] = -2.3 and masses 0.9 - 6M⊙. The models where the 13C burns radiatively (stars of around 2M⊙) produce an overall good match to carbon-enhanced metalpoor (CEMP) stars showing barium enhancements (CEMP-s). On the other hand, none of our models can provide a match to the composition of CEMP stars showing both barium and europium enhancements (CEMP-s/r). The models fail to reproduce the observed Eu abundances, and they also fail to reproduce the correlation between the Eu and Ba abundances. They also cannot match the ratio of heavy-to-light s-process elements observed in many CEMP-s/r stars, which can be more than 10 times higher than in the Solar System. This work has been published [1] and the interested reader should refer to that work for further details, included published tables of yields.

KW - abundances

KW - nuclear reactions

KW - nucleosynthesis

KW - stars: abundances

KW - stars: AGB and post-AGB

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DO - 10.1063/1.4754347

M3 - Conference Paper

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EP - 159

BT - First Stars IV - From Hayashi to the Future

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A2 - Omukai, Kazuyuki

PB - AIP Publishing

CY - USA

T2 - Conference on FIRST STARS - From Hayashi to the Future 2012

Y2 - 21 May 2012 through 25 May 2012

ER -

The s-process at low metallicity

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Keywords

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