Measurement of the Se78(n,γ)Se79 cross section up to 600 keV at the n_TOF facility at CERN

IF 3.4 2区物理与天体物理 Q1 Physics and Astronomy

Physical Review C Pub Date : 2024-12-17 DOI:10.1103/physrevc.110.065805

N. V. Sosnin, C. Lederer-Woods, R. Garg, U. Battino, S. Cristallo, M. Dietz, S. Heinitz, M. Krtička, R. Reifarth, S. Valenta, D. Vescovi, O. Aberle, V. Alcayne, S. Amaducci, J. Andrzejewski, L. Audouin, V. Bécares, V. Babiano-Suárez, M. Bacak, M. Barbagallo, F. Bečvář, G. Bellia, E. Berthoumieux, J. Billowes, D. Bosnar, A. Brown, M. Busso, M. Caamaño, L. Caballero, F. Calviño, M. Calviani, D. Cano-Ott, A. Casanovas, F. Cerutti, Y. H. Chen, E. Chiaveri, N. Colonna, G. Cortés, M. A. Cortés‐Giraldo, L. Coséntino, L. A. Damone, M. Diakaki, C. Domingo-Pardo, R. Dressler, E. Dupont, I. Durán, Z. Eleme, B. Fernández–Domínguez, Andrea Ferrari, P. Finocchiaro, V. Furman, K. Göbel, A. Gawlik-Ramięga, S. Gilardoni, T. Glodariu, I. F. Gonçalves, E. González-Romero, C. Guerrero, F. Gunsing, Hideo Harada, J. Heyse, D. G. Jenkins, E. Jericha, F. Käppeler, Yacine Kadi, Akira Kimura, N. Kivel, M. Kokkoris, Yu. N. Kopatch, D. Kurtulgil, I. Ladarescu, H. Leeb, J. Lerendegui-Marco, S. Lo Meo, S. J. Lonsdale, A. Manna, T. Martínez, A. Masi, C. Massimi, P. Mastinu, M. Mastromarco, F. Matteucci, E. A. Maugeri, A. Mazzone, E. Mendoza, A. Mengoni, V. Michalopoulou, P. M. Milazzo, A. St. J. Murphy, A. Musumarra, A. Negreţ, R. Nolte, F. Ogállar, A. Oprea, N. Patronis, A. Pavlik, J. Perkowski, L. Piersanti, I. Porras, J. Praena, J. M. Quesada, D. Radeck, D. Ramos-Doval, T. Rauscher, D. Rochman, C. Rubbia, M. Sabaté-Gilarte, A. Saxena, P. Schillebeeckx, D. Schumann, A. G. Smith, A. Stamatopoulos, G. Tagliente, J. L. Taı́n, T. Talip, A. Tarifeño-Saldivia, L. Tassan-Gôt, P. Torres-Sánchez, A. Tsinganis, J. Ulrich, S. Urlaß, G. Vannini, V. Variale, P. Vaz, A. Ventura, V. Vlachoudis, R. Vlastou, A. Wallner, P. J. Woods, T. Wright, P. Žugec

{"title":"Measurement of the <mml:math xmlns:mml=\"http://www.w3.org/1998/Math/MathML\"><mml:mrow><mml:mmultiscripts><mml:mi>Se</mml:mi><mml:mprescripts/><mml:none/><mml:mn>78</mml:mn></mml:mmultiscripts><mml:mo>(</mml:mo><mml:mi>n</mml:mi><mml:mo>,</mml:mo><mml:mi>γ</mml:mi><mml:mo>)</mml:mo><mml:mmultiscripts><mml:mi>Se</mml:mi><mml:mprescripts/><mml:none/><mml:mn>79</mml:mn></mml:mmultiscripts></mml:mrow></mml:math> cross section up to 600 keV at the n_TOF facility at CERN","authors":"N. V. Sosnin, C. Lederer-Woods, R. Garg, U. Battino, S. Cristallo, M. Dietz, S. Heinitz, M. Krtička, R. Reifarth, S. Valenta, D. Vescovi, O. Aberle, V. Alcayne, S. Amaducci, J. Andrzejewski, L. Audouin, V. Bécares, V. Babiano-Suárez, M. Bacak, M. Barbagallo, F. Bečvář, G. Bellia, E. Berthoumieux, J. Billowes, D. Bosnar, A. Brown, M. Busso, M. Caamaño, L. Caballero, F. Calviño, M. Calviani, D. Cano-Ott, A. Casanovas, F. Cerutti, Y. H. Chen, E. Chiaveri, N. Colonna, G. Cortés, M. A. Cortés‐Giraldo, L. Coséntino, L. A. Damone, M. Diakaki, C. Domingo-Pardo, R. Dressler, E. Dupont, I. Durán, Z. Eleme, B. Fernández–Domínguez, Andrea Ferrari, P. Finocchiaro, V. Furman, K. Göbel, A. Gawlik-Ramięga, S. Gilardoni, T. Glodariu, I. F. Gonçalves, E. González-Romero, C. Guerrero, F. Gunsing, Hideo Harada, J. Heyse, D. G. Jenkins, E. Jericha, F. Käppeler, Yacine Kadi, Akira Kimura, N. Kivel, M. Kokkoris, Yu. N. Kopatch, D. Kurtulgil, I. Ladarescu, H. Leeb, J. Lerendegui-Marco, S. Lo Meo, S. J. Lonsdale, A. Manna, T. Martínez, A. Masi, C. Massimi, P. Mastinu, M. Mastromarco, F. Matteucci, E. A. Maugeri, A. Mazzone, E. Mendoza, A. Mengoni, V. Michalopoulou, P. M. Milazzo, A. St. J. Murphy, A. Musumarra, A. Negreţ, R. Nolte, F. Ogállar, A. Oprea, N. Patronis, A. Pavlik, J. Perkowski, L. Piersanti, I. Porras, J. Praena, J. M. Quesada, D. Radeck, D. Ramos-Doval, T. Rauscher, D. Rochman, C. Rubbia, M. Sabaté-Gilarte, A. Saxena, P. Schillebeeckx, D. Schumann, A. G. Smith, A. Stamatopoulos, G. Tagliente, J. L. Taı́n, T. Talip, A. Tarifeño-Saldivia, L. Tassan-Gôt, P. Torres-Sánchez, A. Tsinganis, J. Ulrich, S. Urlaß, G. Vannini, V. Variale, P. Vaz, A. Ventura, V. Vlachoudis, R. Vlastou, A. Wallner, P. J. Woods, T. Wright, P. Žugec","doi":"10.1103/physrevc.110.065805","DOIUrl":null,"url":null,"abstract":"The <a:math xmlns:a=\"http://www.w3.org/1998/Math/MathML\"><a:mrow><a:mmultiscripts><a:mi>Se</a:mi><a:mprescripts/><a:none/><a:mn>78</a:mn></a:mmultiscripts><a:mo>(</a:mo><a:mi>n</a:mi><a:mo>,</a:mo><a:mi>γ</a:mi><a:mo>)</a:mo><a:mmultiscripts><a:mi>Se</a:mi><a:mprescripts/><a:none/><a:mn>79</a:mn></a:mmultiscripts></a:mrow></a:math> cross section has a high impact on the abundances of <b:math xmlns:b=\"http://www.w3.org/1998/Math/MathML\"><b:mmultiscripts><b:mi>Se</b:mi><b:mprescripts/><b:none/><b:mn>78</b:mn></b:mmultiscripts></b:math> produced during the slow neutron capture process (<c:math xmlns:c=\"http://www.w3.org/1998/Math/MathML\"><c:mi>s</c:mi></c:math> process) in massive stars. A measurement of the <d:math xmlns:d=\"http://www.w3.org/1998/Math/MathML\"><d:mmultiscripts><d:mi>Se</d:mi><d:mprescripts/><d:none/><d:mn>78</d:mn></d:mmultiscripts></d:math> radiative neutron capture cross section has been performed at the Neutron Time-of-Flight facility at CERN using a set of liquid scintillation detectors that have been optimized for a low sensitivity to neutrons. We present resonance capture kernels up to 70 keV and cross section from 70 to 600 keV. Maxwellian-averaged cross section (MACS) values were calculated for stellar temperatures between <e:math xmlns:e=\"http://www.w3.org/1998/Math/MathML\"><e:mrow><e:mi>k</e:mi><e:mi>T</e:mi><e:mo>=</e:mo><e:mn>5</e:mn></e:mrow></e:math> and 100 keV, with uncertainties between 4.6% and 5.8%. The new MACS values result in substantial decreases of 20–30% of <f:math xmlns:f=\"http://www.w3.org/1998/Math/MathML\"><f:mmultiscripts><f:mi>Se</f:mi><f:mprescripts/><f:none/><f:mn>78</f:mn></f:mmultiscripts></f:math> abundances produced in the <g:math xmlns:g=\"http://www.w3.org/1998/Math/MathML\"><g:mi>s</g:mi></g:math> process in massive stars and AGB stars. Massive stars are now predicted to produce subsolar <h:math xmlns:h=\"http://www.w3.org/1998/Math/MathML\"><h:mrow><h:mmultiscripts><h:mi>Se</h:mi><h:mprescripts/><h:none/><h:mn>78</h:mn></h:mmultiscripts><h:mo>/</h:mo><h:mmultiscripts><h:mi>Se</h:mi><h:mprescripts/><h:none/><h:mn>76</h:mn></h:mmultiscripts></h:mrow></h:math> ratios, which is expected since <i:math xmlns:i=\"http://www.w3.org/1998/Math/MathML\"><i:mmultiscripts><i:mi>Se</i:mi><i:mprescripts/><i:none/><i:mn>76</i:mn></i:mmultiscripts></i:math> is an <j:math xmlns:j=\"http://www.w3.org/1998/Math/MathML\"><j:mi>s</j:mi></j:math>-only isotope, while solar <k:math xmlns:k=\"http://www.w3.org/1998/Math/MathML\"><k:mmultiscripts><k:mi>Se</k:mi><k:mprescripts/><k:none/><k:mn>78</k:mn></k:mmultiscripts></k:math> abundances have also contributions from other nucleosynthesis processes. Published by the American Physical Society 2024","PeriodicalId":20122,"journal":{"name":"Physical Review C","volume":"110 6","pages":""},"PeriodicalIF":3.4000,"publicationDate":"2024-12-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":"2","resultStr":null,"platform":"Semanticscholar","paperid":null,"PeriodicalName":"Physical Review C","FirstCategoryId":"0","ListUrlMain":"https://doi.org/10.1103/physrevc.110.065805","RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":null,"EPubDate":"","PubModel":"","JCR":"Q1","JCRName":"Physics and Astronomy","Score":null,"Total":0}

引用次数: 2

Abstract

The Se78(n,γ)Se79 cross section has a high impact on the abundances of Se78 produced during the slow neutron capture process (s process) in massive stars. A measurement of the Se78 radiative neutron capture cross section has been performed at the Neutron Time-of-Flight facility at CERN using a set of liquid scintillation detectors that have been optimized for a low sensitivity to neutrons. We present resonance capture kernels up to 70 keV and cross section from 70 to 600 keV. Maxwellian-averaged cross section (MACS) values were calculated for stellar temperatures between kT=5 and 100 keV, with uncertainties between 4.6% and 5.8%. The new MACS values result in substantial decreases of 20–30% of Se78 abundances produced in the s process in massive stars and AGB stars. Massive stars are now predicted to produce subsolar Se78/Se76 ratios, which is expected since Se76 is an s-only isotope, while solar Se78 abundances have also contributions from other nucleosynthesis processes. Published by the American Physical Society 2024

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在欧洲核子研究中心n_TOF装置上测量高达600 keV的Se78(n,γ)Se79横截面

Se78(n,γ)Se79截面对大质量恒星在慢中子俘获过程（s过程）中产生的Se78丰度有很大影响。在欧洲核子研究中心的中子飞行时间设施中，使用一套液体闪烁探测器对Se78辐射中子捕获截面进行了测量，该探测器对中子的灵敏度较低。我们提出了高达70 keV的共振捕获核和70至600 keV的截面。计算了恒星温度在kT=5 ~ 100 keV之间的麦克斯韦平均截面（MACS）值，不确定性在4.6% ~ 5.8%之间。新的MACS值导致大质量恒星和AGB恒星在s过程中产生的Se78丰度大幅减少20-30%。现在预计大质量恒星会产生亚太阳Se78/Se76比率，因为Se76是一种纯s同位素，而太阳Se78丰度也有其他核合成过程的贡献。2024年由美国物理学会出版

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来源期刊

Physical Review C 物理-物理：核物理

CiteScore

5.70

自引率

35.50%

发文量

审稿时长

1-2 weeks

期刊介绍： Physical Review C (PRC) is a leading journal in theoretical and experimental nuclear physics, publishing more than two-thirds of the research literature in the field. PRC covers experimental and theoretical results in all aspects of nuclear physics, including: Nucleon-nucleon interaction, few-body systems Nuclear structure Nuclear reactions Relativistic nuclear collisions Hadronic physics and QCD Electroweak interaction, symmetries Nuclear astrophysics