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

^*Corresponding author for this work

Research output: Chapter in Book/Report/Conference proceeding › Conference contribution › peer-review

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 -
Pages	156-159
Number of pages	4
DOIs	https://doi.org/10.1063/1.4754347
Publication status	Published - 2012
Event	1st Stars IV: From Hayashi to the Future - Kyoto, Japan Duration: 21 May 2012 → 25 May 2012

Publication series

Name	AIP Conference Proceedings
Volume	1480
ISSN (Print)	0094-243X
ISSN (Electronic)	1551-7616

Conference

Conference	1st Stars IV: From Hayashi to the Future
Country/Territory	Japan
City	Kyoto
Period	21/05/12 → 25/05/12

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10.1063/1.4754347

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@inproceedings{8654509fd4d04eabb3f35897043ee169,

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: AGB and post-AGB, stars: abundances",

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",

pages = "156--159",

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

note = "1st Stars IV: From Hayashi to the Future ; Conference date: 21-05-2012 Through 25-05-2012",

}

TY - GEN

T1 - The s-process at low metallicity

AU - Stancliffe, Richard J.

AU - Lugaro, Maria A.

AU - Karakas, Amanda I.

AU - Rijs, Carlos

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: AGB and post-AGB

KW - stars: abundances

UR - http://www.scopus.com/inward/record.url?scp=84875530362&partnerID=8YFLogxK

U2 - 10.1063/1.4754347

DO - 10.1063/1.4754347

M3 - Conference contribution

SN - 9780735410923

T3 - AIP Conference Proceedings

SP - 156

EP - 159

BT - First Stars IV - From Hayashi to the Future -

T2 - 1st Stars IV: From Hayashi to the Future

Y2 - 21 May 2012 through 25 May 2012

ER -

The s-process at low metallicity

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Conference

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