Measurement of the ^{140}Ce(n,γ) Cross Section at n_TOF and Its Astrophysical Implications for the Chemical Evolution of the Universe

(n_TOF Collaboration); Thomas Rauscher

doi:10.1103/PhysRevLett.132.122701

Measurement of the ^{140}Ce(n,γ) Cross Section at n_TOF and Its Astrophysical Implications for the Chemical Evolution of the Universe

(n_TOF Collaboration), Thomas Rauscher

Research output: Contribution to journal › Article › peer-review

Abstract

^{140}Ce(n,γ) is a key reaction for slow neutron-capture (s-process) nucleosynthesis due to being a bottleneck in the reaction flow. For this reason, it was measured with high accuracy (uncertainty ≈5%) at the n_TOF facility, with an unprecedented combination of a high purity sample and low neutron-sensitivity detectors. The measured Maxwellian averaged cross section is up to 40% higher than previously accepted values. Stellar model calculations indicate a reduction around 20% of the s-process contribution to the Galactic cerium abundance and smaller sizeable differences for most of the heavier elements. No variations are found in the nucleosynthesis from massive stars.

Original language	English
Article number	122701
Pages (from-to)	1-8
Number of pages	8
Journal	Physical Review Letters
Volume	132
Issue number	12
DOIs	https://doi.org/10.1103/PhysRevLett.132.122701
Publication status	Published - 21 Mar 2024

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© 2024 The Author(s). Published by the American Physical Society. This is an open access article distributed under the terms of the Creative Commons Attribution License (CC BY), https://creativecommons.org/licenses/by/4.0/
Final published version, 599 KBLicence: CC BY

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@article{61ac5c7cdd7646f4b54439d9e24a6926,

title = "Measurement of the ^{140}Ce(n,γ) Cross Section at n_TOF and Its Astrophysical Implications for the Chemical Evolution of the Universe",

abstract = "^{140}Ce(n,γ) is a key reaction for slow neutron-capture (s-process) nucleosynthesis due to being a bottleneck in the reaction flow. For this reason, it was measured with high accuracy (uncertainty ≈5%) at the n_TOF facility, with an unprecedented combination of a high purity sample and low neutron-sensitivity detectors. The measured Maxwellian averaged cross section is up to 40% higher than previously accepted values. Stellar model calculations indicate a reduction around 20% of the s-process contribution to the Galactic cerium abundance and smaller sizeable differences for most of the heavier elements. No variations are found in the nucleosynthesis from massive stars.",

author = "{(n_TOF Collaboration)} and S. Amaducci and N. Colonna and L. Cosentino and S. Cristallo and P. Finocchiaro and M. Krti{\v c}ka and C. Massimi and M. Mastromarco and A. Mazzone and Maugeri, {E. A.} and A. Mengoni and Roederer, {I. U.} and O. Straniero and S. Valenta and D. Vescovi and O. Aberle and V. Alcayne and J. Andrzejewski and L. Audouin and V. Babiano-Suarez and M. Bacak and M. Barbagallo and S. Bennett and E. Berthoumieux and J. Billowes and D. Bosnar and A. Brown and M. Busso and M. Caama{\~n}o and L. Caballero-Ontanaya and F. Calvi{\~n}o and M. Calviani and D. Cano-Ott and A. Casanovas and F. Cerutti and E. Chiaveri and G. Cort{\'e}s and Cort{\'e}s-Giraldo, {M. A.} and Damone, {L. A.} and Davies, {P. J.} and M. Diakaki and M. Dietz and C. Domingo-Pardo and R. Dressler and Q. Ducasse and E. Dupont and I. Dur{\'a}n and Z. Eleme and B. Fern{\'a}ndez-Dom{\'i}nguez and A. Ferrari and V. Furman and K. G{\"o}bel and R. Garg and A. Gawlik-Rami{\c e}ga and S. Gilardoni and Gon{\c c}alves, {I. F.} and E. Gonz{\'a}lez-Romero and C. Guerrero and F. Gunsing and H. Harada and S. Heinitz and J. Heyse and Jenkins, {D. G.} and Junghans, {A. R.} and F. K{\"a}ppeler and Y. Kadi and A. Kimura and I. Knapova and M. Kokkoris and Y. Kopatch and D. Kurtulgil and I. Ladarescu and C. Lederer-Woods and H. Leeb and J. Lerendegui-Marco and Lonsdale, {S. J.} and D. Macina and A. Manna and T. Mart{\'i}nez and A. Masi and P. Mastinu and E. Mendoza and V. Michalopoulou and Milazzo, {P. M.} and F. Mingrone and J. Moreno-Soto and A. Musumarra and A. Negret and R. Nolte and F. Og{\'a}llar and A. Oprea and N. Patronis and A. Pavlik and J. Perkowski and C. Petrone and L. Piersanti and E. Pirovano and I. Porras and J. Praena and Quesada, {J. M.} and D. Ramos-Doval and Thomas Rauscher and R. Reifarth and D. Rochman and C Rubbia and M. Sabat{\'e}-Gilarte and A. Saxena and P. Schillebeeckx and D. Schumann and A. Sekhar and Smith, {A. G.} and Sosnin, {N. V.} and P. Sprung and A. Stamatopoulos and G. Tagliente and Tain, {J. L.} and A. Tarife{\~n}o-Saldivia and Tassan-Got, {Laurent L.} and T.H. Thomas and P. Torres-S{\'a}nchez and A. Tsinganis and J. Ulrich and S. Urlass and G. Vannini, and V. Variale and P Vaz and A. Ventura and V. Vlachoudis and R. Vlastou and A. Wallner and Woods, {P. J.} and T. Wright and P. {\v Z}ugec",

note = "{\textcopyright} 2024 The Author(s). Published by the American Physical Society. This is an open access article distributed under the terms of the Creative Commons Attribution License (CC BY), https://creativecommons.org/licenses/by/4.0/",

year = "2024",

month = mar,

day = "21",

doi = "10.1103/PhysRevLett.132.122701",

language = "English",

volume = "132",

pages = "1--8",

journal = "Physical Review Letters",

issn = "0031-9007",

publisher = "American Physical Society (APS)",

number = "12",

}

TY - JOUR

T1 - Measurement of the ^{140}Ce(n,γ) Cross Section at n_TOF and Its Astrophysical Implications for the Chemical Evolution of the Universe

AU - (n_TOF Collaboration)

AU - Amaducci, S.

AU - Colonna, N.

AU - Cosentino, L.

AU - Cristallo, S.

AU - Finocchiaro, P.

AU - Krtička, M.

AU - Massimi, C.

AU - Mastromarco, M.

AU - Mazzone, A.

AU - Maugeri, E. A.

AU - Mengoni, A.

AU - Roederer, I. U.

AU - Straniero, O.

AU - Valenta, S.

AU - Vescovi, D.

AU - Aberle, O.

AU - Alcayne, V.

AU - Andrzejewski, J.

AU - Audouin, L.

AU - Babiano-Suarez, V.

AU - Bacak, M.

AU - Barbagallo, M.

AU - Bennett, S.

AU - Berthoumieux, E.

AU - Billowes, J.

AU - Bosnar, D.

AU - Brown, A.

AU - Busso, M.

AU - Caamaño, M.

AU - Caballero-Ontanaya, L.

AU - Calviño, F.

AU - Calviani, M.

AU - Cano-Ott, D.

AU - Casanovas, A.

AU - Cerutti, F.

AU - Chiaveri, E.

AU - Cortés, G.

AU - Cortés-Giraldo, M. A.

AU - Damone, L. A.

AU - Davies, P. J.

AU - Diakaki, M.

AU - Dietz, M.

AU - Domingo-Pardo, C.

AU - Dressler, R.

AU - Ducasse, Q.

AU - Dupont, E.

AU - Durán, I.

AU - Eleme, Z.

AU - Fernández-Domínguez, B.

AU - Ferrari, A.

AU - Furman, V.

AU - Göbel, K.

AU - Garg, R.

AU - Gawlik-Ramięga, A.

AU - Gilardoni, S.

AU - Gonçalves, I. F.

AU - González-Romero, E.

AU - Guerrero, C.

AU - Gunsing, F.

AU - Harada, H.

AU - Heinitz, S.

AU - Heyse, J.

AU - Jenkins, D. G.

AU - Junghans, A. R.

AU - Käppeler, F.

AU - Kadi, Y.

AU - Kimura, A.

AU - Knapova, I.

AU - Kokkoris, M.

AU - Kopatch, Y.

AU - Kurtulgil, D.

AU - Ladarescu, I.

AU - Lederer-Woods, C.

AU - Leeb, H.

AU - Lerendegui-Marco, J.

AU - Lonsdale, S. J.

AU - Macina, D.

AU - Manna, A.

AU - Martínez, T.

AU - Masi, A.

AU - Mastinu, P.

AU - Mendoza, E.

AU - Michalopoulou, V.

AU - Milazzo, P. M.

AU - Mingrone, F.

AU - Moreno-Soto, J.

AU - Musumarra, A.

AU - Negret, A.

AU - Nolte, R.

AU - Ogállar, F.

AU - Oprea, A.

AU - Patronis, N.

AU - Pavlik, A.

AU - Perkowski, J.

AU - Petrone, C.

AU - Piersanti, L.

AU - Pirovano, E.

AU - Porras, I.

AU - Praena, J.

AU - Quesada, J. M.

AU - Ramos-Doval, D.

AU - Rauscher, Thomas

AU - Reifarth, R.

AU - Rochman, D.

AU - Rubbia, C

AU - Sabaté-Gilarte, M.

AU - Saxena, A.

AU - Schillebeeckx, P.

AU - Schumann, D.

AU - Sekhar, A.

AU - Smith, A. G.

AU - Sosnin, N. V.

AU - Sprung, P.

AU - Stamatopoulos, A.

AU - Tagliente, G.

AU - Tain, J. L.

AU - Tarifeño-Saldivia, A.

AU - Tassan-Got, Laurent L.

AU - Thomas, T.H.

AU - Torres-Sánchez, P.

AU - Tsinganis, A.

AU - Ulrich, J.

AU - Urlass, S.

AU - Vannini,, G.

AU - Variale, V.

AU - Vaz, P

AU - Ventura, A.

AU - Vlachoudis, V.

AU - Vlastou, R.

AU - Wallner, A.

AU - Woods, P. J.

AU - Wright, T.

AU - Žugec, P.

N1 - © 2024 The Author(s). Published by the American Physical Society. This is an open access article distributed under the terms of the Creative Commons Attribution License (CC BY), https://creativecommons.org/licenses/by/4.0/

PY - 2024/3/21

Y1 - 2024/3/21

N2 - ^{140}Ce(n,γ) is a key reaction for slow neutron-capture (s-process) nucleosynthesis due to being a bottleneck in the reaction flow. For this reason, it was measured with high accuracy (uncertainty ≈5%) at the n_TOF facility, with an unprecedented combination of a high purity sample and low neutron-sensitivity detectors. The measured Maxwellian averaged cross section is up to 40% higher than previously accepted values. Stellar model calculations indicate a reduction around 20% of the s-process contribution to the Galactic cerium abundance and smaller sizeable differences for most of the heavier elements. No variations are found in the nucleosynthesis from massive stars.

AB - ^{140}Ce(n,γ) is a key reaction for slow neutron-capture (s-process) nucleosynthesis due to being a bottleneck in the reaction flow. For this reason, it was measured with high accuracy (uncertainty ≈5%) at the n_TOF facility, with an unprecedented combination of a high purity sample and low neutron-sensitivity detectors. The measured Maxwellian averaged cross section is up to 40% higher than previously accepted values. Stellar model calculations indicate a reduction around 20% of the s-process contribution to the Galactic cerium abundance and smaller sizeable differences for most of the heavier elements. No variations are found in the nucleosynthesis from massive stars.

UR - http://www.scopus.com/inward/record.url?scp=85188670848&partnerID=8YFLogxK

U2 - 10.1103/PhysRevLett.132.122701

DO - 10.1103/PhysRevLett.132.122701

M3 - Article

C2 - 38579210

AN - SCOPUS:85188670848

SN - 0031-9007

VL - 132

SP - 1

EP - 8

JO - Physical Review Letters

JF - Physical Review Letters

IS - 12

M1 - 122701

ER -

Measurement of the ^{140}Ce(n,γ) Cross Section at n_TOF and Its Astrophysical Implications for the Chemical Evolution of the Universe

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