S-process Nucleosynthesis in SAGB Stars

H H B Lau, Carolyn Doherty, Pilar Gil-Pons, John Charles Lattanzio

Research output: Chapter in Book/Report/Conference proceedingConference PaperResearch

Abstract

Super asymptotic giant branch (SAGB) stars, in a mass range between 5 and 11 M, have a similar evolution to high-mass AGB stars but are hot enough to ignite carbon in their cores non-degenerately during the early AGB phase. However, they could have a different nucleosynthesis signature because of the higher temperature at the bottom of intershell convective zone. In particular, 22Ne is the major source of neutrons. We have used the new Monash nucleosynthesis code MONTAGE to compute yields of 475 different isotopes, including s-process elements. We find 22Ne is the major source of neutrons and the 13C contribution is not significant. Moreover, the reaction rate of the triple-alpha reaction and 12C(α, γ)16O is critical to determine the nucleosynthesis of SAGB stars, particularly the heavy s-process isotopes and Pb.
Original languageEnglish
Title of host publicationWhy Galaxies Care about AGB Stars II: Shining Examples and Common Inhabitants
Subtitle of host publicationProceedings of a conference held at University Campus, Vienna, Austria 16-20 August 2010
EditorsF Kerschbaum, T Lebzelter, R F Wing
Place of PublicationSan Francisco CA USA
PublisherAstronomical Society of the Pacific
Pages45-50
Number of pages6
Volume445
Edition1
Publication statusPublished - 2011

Publication series

NameAstronomical Society of the Pacific Conference Series
PublisherAstronomical Society of the Pacific
Number1
Volume445

Cite this

Lau, H. H. B., Doherty, C., Gil-Pons, P., & Lattanzio, J. C. (2011). S-process Nucleosynthesis in SAGB Stars. In F. Kerschbaum, T. Lebzelter, & R. F. Wing (Eds.), Why Galaxies Care about AGB Stars II: Shining Examples and Common Inhabitants: Proceedings of a conference held at University Campus, Vienna, Austria 16-20 August 2010 (1 ed., Vol. 445, pp. 45-50). (Astronomical Society of the Pacific Conference Series; Vol. 445, No. 1). San Francisco CA USA: Astronomical Society of the Pacific.
Lau, H H B ; Doherty, Carolyn ; Gil-Pons, Pilar ; Lattanzio, John Charles. / S-process Nucleosynthesis in SAGB Stars. Why Galaxies Care about AGB Stars II: Shining Examples and Common Inhabitants: Proceedings of a conference held at University Campus, Vienna, Austria 16-20 August 2010. editor / F Kerschbaum ; T Lebzelter ; R F Wing. Vol. 445 1. ed. San Francisco CA USA : Astronomical Society of the Pacific, 2011. pp. 45-50 (Astronomical Society of the Pacific Conference Series; 1).
@inproceedings{d633c4d1a048453a972fc6999e61c917,
title = "S-process Nucleosynthesis in SAGB Stars",
abstract = "Super asymptotic giant branch (SAGB) stars, in a mass range between 5 and 11 M, have a similar evolution to high-mass AGB stars but are hot enough to ignite carbon in their cores non-degenerately during the early AGB phase. However, they could have a different nucleosynthesis signature because of the higher temperature at the bottom of intershell convective zone. In particular, 22Ne is the major source of neutrons. We have used the new Monash nucleosynthesis code MONTAGE to compute yields of 475 different isotopes, including s-process elements. We find 22Ne is the major source of neutrons and the 13C contribution is not significant. Moreover, the reaction rate of the triple-alpha reaction and 12C(α, γ)16O is critical to determine the nucleosynthesis of SAGB stars, particularly the heavy s-process isotopes and Pb.",
author = "Lau, {H H B} and Carolyn Doherty and Pilar Gil-Pons and Lattanzio, {John Charles}",
year = "2011",
language = "English",
volume = "445",
series = "Astronomical Society of the Pacific Conference Series",
publisher = "Astronomical Society of the Pacific",
number = "1",
pages = "45--50",
editor = "F Kerschbaum and T Lebzelter and Wing, {R F}",
booktitle = "Why Galaxies Care about AGB Stars II: Shining Examples and Common Inhabitants",
address = "United States of America",
edition = "1",

}

Lau, HHB, Doherty, C, Gil-Pons, P & Lattanzio, JC 2011, S-process Nucleosynthesis in SAGB Stars. in F Kerschbaum, T Lebzelter & RF Wing (eds), Why Galaxies Care about AGB Stars II: Shining Examples and Common Inhabitants: Proceedings of a conference held at University Campus, Vienna, Austria 16-20 August 2010. 1 edn, vol. 445, Astronomical Society of the Pacific Conference Series, no. 1, vol. 445, Astronomical Society of the Pacific, San Francisco CA USA, pp. 45-50.

S-process Nucleosynthesis in SAGB Stars. / Lau, H H B; Doherty, Carolyn; Gil-Pons, Pilar; Lattanzio, John Charles.

Why Galaxies Care about AGB Stars II: Shining Examples and Common Inhabitants: Proceedings of a conference held at University Campus, Vienna, Austria 16-20 August 2010. ed. / F Kerschbaum; T Lebzelter; R F Wing. Vol. 445 1. ed. San Francisco CA USA : Astronomical Society of the Pacific, 2011. p. 45-50 (Astronomical Society of the Pacific Conference Series; Vol. 445, No. 1).

Research output: Chapter in Book/Report/Conference proceedingConference PaperResearch

TY - GEN

T1 - S-process Nucleosynthesis in SAGB Stars

AU - Lau, H H B

AU - Doherty, Carolyn

AU - Gil-Pons, Pilar

AU - Lattanzio, John Charles

PY - 2011

Y1 - 2011

N2 - Super asymptotic giant branch (SAGB) stars, in a mass range between 5 and 11 M, have a similar evolution to high-mass AGB stars but are hot enough to ignite carbon in their cores non-degenerately during the early AGB phase. However, they could have a different nucleosynthesis signature because of the higher temperature at the bottom of intershell convective zone. In particular, 22Ne is the major source of neutrons. We have used the new Monash nucleosynthesis code MONTAGE to compute yields of 475 different isotopes, including s-process elements. We find 22Ne is the major source of neutrons and the 13C contribution is not significant. Moreover, the reaction rate of the triple-alpha reaction and 12C(α, γ)16O is critical to determine the nucleosynthesis of SAGB stars, particularly the heavy s-process isotopes and Pb.

AB - Super asymptotic giant branch (SAGB) stars, in a mass range between 5 and 11 M, have a similar evolution to high-mass AGB stars but are hot enough to ignite carbon in their cores non-degenerately during the early AGB phase. However, they could have a different nucleosynthesis signature because of the higher temperature at the bottom of intershell convective zone. In particular, 22Ne is the major source of neutrons. We have used the new Monash nucleosynthesis code MONTAGE to compute yields of 475 different isotopes, including s-process elements. We find 22Ne is the major source of neutrons and the 13C contribution is not significant. Moreover, the reaction rate of the triple-alpha reaction and 12C(α, γ)16O is critical to determine the nucleosynthesis of SAGB stars, particularly the heavy s-process isotopes and Pb.

M3 - Conference Paper

VL - 445

T3 - Astronomical Society of the Pacific Conference Series

SP - 45

EP - 50

BT - Why Galaxies Care about AGB Stars II: Shining Examples and Common Inhabitants

A2 - Kerschbaum, F

A2 - Lebzelter, T

A2 - Wing, R F

PB - Astronomical Society of the Pacific

CY - San Francisco CA USA

ER -

Lau HHB, Doherty C, Gil-Pons P, Lattanzio JC. S-process Nucleosynthesis in SAGB Stars. In Kerschbaum F, Lebzelter T, Wing RF, editors, Why Galaxies Care about AGB Stars II: Shining Examples and Common Inhabitants: Proceedings of a conference held at University Campus, Vienna, Austria 16-20 August 2010. 1 ed. Vol. 445. San Francisco CA USA: Astronomical Society of the Pacific. 2011. p. 45-50. (Astronomical Society of the Pacific Conference Series; 1).