1
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deBoer RJ, Febbraro M, Bardayan DW, Boomershine C, Brandenburg K, Brune C, Coil S, Couder M, Derkin J, Dede S, Fang R, Fritsch A, Gula A, Gyürky G, Hackett B, Hamad G, Jones-Alberty Y, Kelmar R, Manukyan K, Matney M, McDonaugh J, Meisel Z, Moylan S, Nattress J, Odell D, O'Malley P, Paris MW, Robertson D, Shahina, Singh N, Smith K, Smith MS, Stech E, Tan W, Wiescher M. Measurement of the ^{13}C(α, n_{0})^{16}O Differential Cross Section from 0.8 to 6.5 MeV. Phys Rev Lett 2024; 132:062702. [PMID: 38394565 DOI: 10.1103/physrevlett.132.062702] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 03/18/2023] [Revised: 09/05/2023] [Accepted: 01/17/2024] [Indexed: 02/25/2024]
Abstract
The cross section of the ^{13}C(α,n)^{16}O reaction is needed for nuclear astrophysics and applications to a precision of 10% or better, yet inconsistencies among 50 years of experimental studies currently lead to an uncertainty of ≈15%. Using a state-of-the-art neutron detection array, we have performed a high resolution differential cross section study covering a broad energy range. These measurements result in a dramatic improvement in the extrapolation of the cross section to stellar energies potentially reducing the uncertainty to ≈5% and resolving long standing discrepancies in higher energy data.
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Affiliation(s)
- R J deBoer
- Department of Physics and Astronomy, University of Notre Dame, Notre Dame, Indiana 46556, USA
| | - M Febbraro
- Oak Ridge National Laboratory, Oak Ridge, Tennessee 37831, USA
| | - D W Bardayan
- Department of Physics and Astronomy, University of Notre Dame, Notre Dame, Indiana 46556, USA
| | - C Boomershine
- Department of Physics and Astronomy, University of Notre Dame, Notre Dame, Indiana 46556, USA
| | - K Brandenburg
- Department of Physics and Astronomy, Ohio University, Athens, Ohio 45701, USA
| | - C Brune
- Department of Physics and Astronomy, Ohio University, Athens, Ohio 45701, USA
| | - S Coil
- Department of Physics and Astronomy, University of Notre Dame, Notre Dame, Indiana 46556, USA
| | - M Couder
- Department of Physics and Astronomy, University of Notre Dame, Notre Dame, Indiana 46556, USA
| | - J Derkin
- Department of Physics and Astronomy, Ohio University, Athens, Ohio 45701, USA
| | - S Dede
- Department of Physics and Astronomy, University of Notre Dame, Notre Dame, Indiana 46556, USA
| | - R Fang
- Department of Physics and Astronomy, University of Notre Dame, Notre Dame, Indiana 46556, USA
| | - A Fritsch
- Department of Physics, Gonzaga University, Spokane, Washington 99258, USA
| | - A Gula
- Department of Physics and Astronomy, University of Notre Dame, Notre Dame, Indiana 46556, USA
| | - Gy Gyürky
- Institute for Nuclear Research (Atomki), P.O.B 51, H-4001 Debrecen, Hungary
| | - B Hackett
- Department of Physics and Astronomy, University of Tennessee, Knoxville, Tennessee 37996, USA
| | - G Hamad
- Department of Physics and Astronomy, Ohio University, Athens, Ohio 45701, USA
| | - Y Jones-Alberty
- Department of Physics and Astronomy, Ohio University, Athens, Ohio 45701, USA
| | - R Kelmar
- Department of Physics and Astronomy, University of Notre Dame, Notre Dame, Indiana 46556, USA
| | - K Manukyan
- Department of Physics and Astronomy, University of Notre Dame, Notre Dame, Indiana 46556, USA
| | - M Matney
- Department of Physics and Astronomy, University of Notre Dame, Notre Dame, Indiana 46556, USA
| | - J McDonaugh
- Department of Physics and Astronomy, University of Notre Dame, Notre Dame, Indiana 46556, USA
| | - Z Meisel
- Department of Physics and Astronomy, Ohio University, Athens, Ohio 45701, USA
| | - S Moylan
- Department of Physics and Astronomy, University of Notre Dame, Notre Dame, Indiana 46556, USA
| | - J Nattress
- Oak Ridge National Laboratory, Oak Ridge, Tennessee 37831, USA
| | - D Odell
- Department of Physics and Astronomy, Ohio University, Athens, Ohio 45701, USA
| | - P O'Malley
- Department of Physics and Astronomy, University of Notre Dame, Notre Dame, Indiana 46556, USA
| | - M W Paris
- Theoretical Division, Los Alamos National Laboratory, Los Alamos, New Mexico 87545, USA
| | - D Robertson
- Department of Physics and Astronomy, University of Notre Dame, Notre Dame, Indiana 46556, USA
| | - Shahina
- Department of Physics and Astronomy, University of Notre Dame, Notre Dame, Indiana 46556, USA
| | - N Singh
- Department of Physics and Astronomy, Ohio University, Athens, Ohio 45701, USA
| | - K Smith
- Los Alamos National Laboratory, Los Alamos, New Mexico 87545, USA
| | - M S Smith
- Oak Ridge National Laboratory, Oak Ridge, Tennessee 37831, USA
| | - E Stech
- Department of Physics and Astronomy, University of Notre Dame, Notre Dame, Indiana 46556, USA
| | - W Tan
- Department of Physics and Astronomy, University of Notre Dame, Notre Dame, Indiana 46556, USA
| | - M Wiescher
- Department of Physics and Astronomy, University of Notre Dame, Notre Dame, Indiana 46556, USA
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2
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Skowronski J, Boeltzig A, Ciani GF, Csedreki L, Piatti D, Aliotta M, Ananna C, Barile F, Bemmerer D, Best A, Broggini C, Bruno CG, Caciolli A, Campostrini M, Cavanna F, Colombetti P, Compagnucci A, Corvisiero P, Davinson T, Depalo R, Di Leva A, Elekes Z, Ferraro F, Formicola A, Fülöp Z, Gervino G, Gesuè RM, Guglielmetti A, Gustavino C, Gyürky G, Imbriani G, Junker M, Lugaro M, Marigo P, Masha E, Menegazzo R, Paticchio V, Perrino R, Prati P, Rapagnani D, Rigato V, Schiavulli L, Sidhu RS, Straniero O, Szücs T, Zavatarelli S. Proton-Capture Rates on Carbon Isotopes and Their Impact on the Astrophysical ^{12}C/^{13}C Ratio. Phys Rev Lett 2023; 131:162701. [PMID: 37925687 DOI: 10.1103/physrevlett.131.162701] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 01/23/2023] [Revised: 05/03/2023] [Accepted: 07/13/2023] [Indexed: 11/07/2023]
Abstract
The ^{12}C/^{13}C ratio is a significant indicator of nucleosynthesis and mixing processes during hydrogen burning in stars. Its value mainly depends on the relative rates of the ^{12}C(p,γ)^{13}N and ^{13}C(p,γ)^{14}N reactions. Both reactions have been studied at the Laboratory for Underground Nuclear Astrophysics (LUNA) in Italy down to the lowest energies to date (E_{c.m.}=60 keV) reaching for the first time the high energy tail of hydrogen burning in the shell of giant stars. Our cross sections, obtained with both prompt γ-ray detection and activation measurements, are the most precise to date with overall systematic uncertainties of 7%-8%. Compared with most of the literature, our results are systematically lower, by 25% for the ^{12}C(p,γ)^{13}N reaction and by 30% for ^{13}C(p,γ)^{14}N. We provide the most precise value up to now of 3.6±0.4 in the 20-140 MK range for the lowest possible ^{12}C/^{13}C ratio that can be produced during H burning in giant stars.
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Affiliation(s)
- J Skowronski
- Dipartimento di Fisica, Università degli Studi di Padova, 35131 Padova, Italy
- INFN, Sezione di Padova, 35131 Padova, Italy
| | - A Boeltzig
- Helmholtz-Zentrum Dresden-Rossendorf, 01328 Dresden, Germany
- INFN, Laboratori Nazionali del Gran Sasso, 67100 Assergi, Italy
- Dipartimento di Fisica "E. Pancini," Università degli Studi di Napoli "Federico II," 80125 Naples, Italy
| | - G F Ciani
- Dipartimento di Fisica "M. Merlin," Università degli Studi di Bari "A. Moro," 70125 Bari, Italy
- INFN, Sezione di Bari, 70125 Bari, Italy
| | - L Csedreki
- Institute for Nuclear Research (ATOMKI), P.O. Box 51, H-4001 Debrecen, Hungary
| | - D Piatti
- Dipartimento di Fisica, Università degli Studi di Padova, 35131 Padova, Italy
- INFN, Sezione di Padova, 35131 Padova, Italy
| | - M Aliotta
- SUPA, School of Physics and Astronomy, University of Edinburgh, EH9 3FD Edinburgh, United Kingdom
| | - C Ananna
- Dipartimento di Fisica "E. Pancini," Università degli Studi di Napoli "Federico II," 80125 Naples, Italy
- INFN, Sezione di Napoli, 80125 Naples, Italy
| | - F Barile
- Dipartimento di Fisica "M. Merlin," Università degli Studi di Bari "A. Moro," 70125 Bari, Italy
- INFN, Sezione di Bari, 70125 Bari, Italy
| | - D Bemmerer
- Helmholtz-Zentrum Dresden-Rossendorf, 01328 Dresden, Germany
| | - A Best
- Dipartimento di Fisica "E. Pancini," Università degli Studi di Napoli "Federico II," 80125 Naples, Italy
- INFN, Sezione di Napoli, 80125 Naples, Italy
| | - C Broggini
- INFN, Sezione di Padova, 35131 Padova, Italy
| | - C G Bruno
- SUPA, School of Physics and Astronomy, University of Edinburgh, EH9 3FD Edinburgh, United Kingdom
| | - A Caciolli
- Dipartimento di Fisica, Università degli Studi di Padova, 35131 Padova, Italy
- INFN, Sezione di Padova, 35131 Padova, Italy
| | - M Campostrini
- Laboratori Nazionali di Legnaro, 35020 Legnaro, Italy
| | - F Cavanna
- INFN, Sezione di Torino, 10125 Torino, Italy
| | - P Colombetti
- INFN, Sezione di Torino, 10125 Torino, Italy
- Dipartimento di Fisica, Università degli Studi di Torino, 10125 Torino, Italy
| | - A Compagnucci
- INFN, Laboratori Nazionali del Gran Sasso, 67100 Assergi, Italy
- Gran Sasso Science Institute, 67100 L'Aquila, Italy
| | - P Corvisiero
- Università degli Studi di Genova, 16146 Genova, Italy
- INFN, Sezione di Genova, 16146 Genova, Italy
| | - T Davinson
- SUPA, School of Physics and Astronomy, University of Edinburgh, EH9 3FD Edinburgh, United Kingdom
| | - R Depalo
- Università degli Studi di Milano, 20133 Milano, Italy
- INFN, Sezione di Milano, 20133 Milano, Italy
| | - A Di Leva
- Dipartimento di Fisica "E. Pancini," Università degli Studi di Napoli "Federico II," 80125 Naples, Italy
- INFN, Sezione di Napoli, 80125 Naples, Italy
| | - Z Elekes
- Institute for Nuclear Research (ATOMKI), P.O. Box 51, H-4001 Debrecen, Hungary
| | - F Ferraro
- INFN, Laboratori Nazionali del Gran Sasso, 67100 Assergi, Italy
- Università degli Studi di Milano, 20133 Milano, Italy
| | | | - Zs Fülöp
- Institute for Nuclear Research (ATOMKI), P.O. Box 51, H-4001 Debrecen, Hungary
| | - G Gervino
- INFN, Sezione di Torino, 10125 Torino, Italy
- Dipartimento di Fisica, Università degli Studi di Torino, 10125 Torino, Italy
| | - R M Gesuè
- INFN, Laboratori Nazionali del Gran Sasso, 67100 Assergi, Italy
- Gran Sasso Science Institute, 67100 L'Aquila, Italy
| | - A Guglielmetti
- Università degli Studi di Milano, 20133 Milano, Italy
- INFN, Sezione di Milano, 20133 Milano, Italy
| | | | - Gy Gyürky
- Institute for Nuclear Research (ATOMKI), P.O. Box 51, H-4001 Debrecen, Hungary
| | - G Imbriani
- Dipartimento di Fisica "E. Pancini," Università degli Studi di Napoli "Federico II," 80125 Naples, Italy
- INFN, Sezione di Napoli, 80125 Naples, Italy
| | - M Junker
- INFN, Laboratori Nazionali del Gran Sasso, 67100 Assergi, Italy
| | - M Lugaro
- Konkoly Observatory, Research Centre for Astronomy and Earth Sciences (CSFK), MTA Centre for Excellence, 1121 Budapest, Hungary
- ELTE Eötvös Loránd University, Institute of Physics, 1117 Budapest, Hungary
| | - P Marigo
- Dipartimento di Fisica, Università degli Studi di Padova, 35131 Padova, Italy
- INFN, Sezione di Padova, 35131 Padova, Italy
| | - E Masha
- Helmholtz-Zentrum Dresden-Rossendorf, 01328 Dresden, Germany
- Università degli Studi di Milano, 20133 Milano, Italy
| | - R Menegazzo
- INFN, Sezione di Padova, 35131 Padova, Italy
| | | | - R Perrino
- INFN, Sezione di Bari, 70125 Bari, Italy
| | - P Prati
- Università degli Studi di Genova, 16146 Genova, Italy
- INFN, Sezione di Genova, 16146 Genova, Italy
| | - D Rapagnani
- Dipartimento di Fisica "E. Pancini," Università degli Studi di Napoli "Federico II," 80125 Naples, Italy
- INFN, Sezione di Napoli, 80125 Naples, Italy
| | - V Rigato
- Laboratori Nazionali di Legnaro, 35020 Legnaro, Italy
| | - L Schiavulli
- Dipartimento di Fisica "M. Merlin," Università degli Studi di Bari "A. Moro," 70125 Bari, Italy
- INFN, Sezione di Bari, 70125 Bari, Italy
| | - R S Sidhu
- SUPA, School of Physics and Astronomy, University of Edinburgh, EH9 3FD Edinburgh, United Kingdom
| | - O Straniero
- INFN, Sezione di Roma, 00185 Roma, Italy
- INAF-Osservatorio Astronomico d'Abruzzo, 64100, Teramo, Italy
| | - T Szücs
- Institute for Nuclear Research (ATOMKI), P.O. Box 51, H-4001 Debrecen, Hungary
| | - S Zavatarelli
- Università degli Studi di Genova, 16146 Genova, Italy
- INFN, Sezione di Genova, 16146 Genova, Italy
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3
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Ciani GF, Csedreki L, Rapagnani D, Aliotta M, Balibrea-Correa J, Barile F, Bemmerer D, Best A, Boeltzig A, Broggini C, Bruno CG, Caciolli A, Cavanna F, Chillery T, Colombetti P, Corvisiero P, Cristallo S, Davinson T, Depalo R, Di Leva A, Elekes Z, Ferraro F, Fiore E, Formicola A, Fülöp Z, Gervino G, Guglielmetti A, Gustavino C, Gyürky G, Imbriani G, Junker M, Lugaro M, Marigo P, Masha E, Menegazzo R, Mossa V, Pantaleo FR, Paticchio V, Perrino R, Piatti D, Prati P, Schiavulli L, Stöckel K, Straniero O, Szücs T, Takács MP, Terrasi F, Vescovi D, Zavatarelli S. Direct Measurement of the ^{13}C(α,n)^{16}O Cross Section into the s-Process Gamow Peak. Phys Rev Lett 2021; 127:152701. [PMID: 34677992 DOI: 10.1103/physrevlett.127.152701] [Citation(s) in RCA: 9] [Impact Index Per Article: 3.0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 04/11/2021] [Revised: 06/08/2021] [Accepted: 08/17/2021] [Indexed: 06/13/2023]
Abstract
One of the main neutron sources for the astrophysical s process is the reaction ^{13}C(α,n)^{16}O, taking place in thermally pulsing asymptotic giant branch stars at temperatures around 90 MK. To model the nucleosynthesis during this process the reaction cross section needs to be known in the 150-230 keV energy window (Gamow peak). At these sub-Coulomb energies, cross section direct measurements are severely affected by the low event rate, making us rely on input from indirect methods and extrapolations from higher-energy direct data. This leads to an uncertainty in the cross section at the relevant energies too high to reliably constrain the nuclear physics input to s-process calculations. We present the results from a new deep-underground measurement of ^{13}C(α,n)^{16}O, covering the energy range 230-300 keV, with drastically reduced uncertainties over previous measurements and for the first time providing data directly inside the s-process Gamow peak. Selected stellar models have been computed to estimate the impact of our revised reaction rate. For stars of nearly solar composition, we find sizeable variations of some isotopes, whose production is influenced by the activation of close-by branching points that are sensitive to the neutron density, in particular, the two radioactive nuclei ^{60}Fe and ^{205}Pb, as well as ^{152}Gd.
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Affiliation(s)
- G F Ciani
- Gran Sasso Science Institute, Viale F. Crispi 7, 67100 L'Aquila, Italy
- INFN, Laboratori Nazionali del Gran Sasso (LNGS), 67100 Assergi, Italy
- Institute for Nuclear Research (ATOMKI), P.O. Box 51, HU-4001 Debrecen, Hungary
| | - L Csedreki
- Gran Sasso Science Institute, Viale F. Crispi 7, 67100 L'Aquila, Italy
- INFN, Laboratori Nazionali del Gran Sasso (LNGS), 67100 Assergi, Italy
- Institute for Nuclear Research (ATOMKI), P.O. Box 51, HU-4001 Debrecen, Hungary
| | - D Rapagnani
- Università di Napoli "Federico II," 80126 Napoli, Italy
- INFN, Sezione di Napoli, 80126 Napoli, Italy
| | - M Aliotta
- SUPA, School of Physics and Astronomy, University of Edinburgh, EH9 3FD Edinburgh, United Kingdom
| | - J Balibrea-Correa
- Università di Napoli "Federico II," 80126 Napoli, Italy
- INFN, Sezione di Napoli, 80126 Napoli, Italy
| | - F Barile
- Università degli Studi di Bari, 70121 Bari, Italy
- INFN, Sezione di Bari, 70125 Bari, Italy
| | - D Bemmerer
- Helmholtz-Zentrum Dresden-Rossendorf, Bautzner Landstrasse 400, 01328 Dresden, Germany
| | - A Best
- Università di Napoli "Federico II," 80126 Napoli, Italy
- INFN, Sezione di Napoli, 80126 Napoli, Italy
| | - A Boeltzig
- Università di Napoli "Federico II," 80126 Napoli, Italy
- INFN, Sezione di Napoli, 80126 Napoli, Italy
| | - C Broggini
- INFN, Sezione di Padova, Via F. Marzolo 8, 35131 Padova, Italy
| | - C G Bruno
- SUPA, School of Physics and Astronomy, University of Edinburgh, EH9 3FD Edinburgh, United Kingdom
| | - A Caciolli
- INFN, Sezione di Padova, Via F. Marzolo 8, 35131 Padova, Italy
- Università degli Studi di Padova, Via F. Marzolo 8, 35131 Padova, Italy
| | - F Cavanna
- INFN, Sezione di Torino, Via Pietro Giuria, 1, 10125 Torino, Italy
| | - T Chillery
- SUPA, School of Physics and Astronomy, University of Edinburgh, EH9 3FD Edinburgh, United Kingdom
| | - P Colombetti
- INFN, Sezione di Torino, Via Pietro Giuria, 1, 10125 Torino, Italy
| | - P Corvisiero
- Università degli Studi di Genova, 16126 Genova, Italy
- INFN, Sezione di Genova, Via Dodecaneso 33, 16146 Genova, Italy
| | - S Cristallo
- INAF, Osservatorio Astronomico d'Abruzzo, 64100 Teramo, Italy
- INFN, Sezione of Perugia, Via A. Pascoli snc, 06123 Perugia, Italy
| | - T Davinson
- SUPA, School of Physics and Astronomy, University of Edinburgh, EH9 3FD Edinburgh, United Kingdom
| | - R Depalo
- INFN, Sezione di Padova, Via F. Marzolo 8, 35131 Padova, Italy
- Università degli Studi di Padova, Via F. Marzolo 8, 35131 Padova, Italy
| | - A Di Leva
- Università di Napoli "Federico II," 80126 Napoli, Italy
- INFN, Sezione di Napoli, 80126 Napoli, Italy
| | - Z Elekes
- Institute for Nuclear Research (ATOMKI), P.O. Box 51, HU-4001 Debrecen, Hungary
| | - F Ferraro
- Università degli Studi di Genova, 16126 Genova, Italy
- INFN, Sezione di Genova, Via Dodecaneso 33, 16146 Genova, Italy
| | - E Fiore
- Università degli Studi di Bari, 70121 Bari, Italy
- INFN, Sezione di Bari, 70125 Bari, Italy
| | - A Formicola
- INFN, Laboratori Nazionali del Gran Sasso (LNGS), 67100 Assergi, Italy
| | - Zs Fülöp
- Institute for Nuclear Research (ATOMKI), P.O. Box 51, HU-4001 Debrecen, Hungary
| | - G Gervino
- Università degli Studi di Torino, 10125 Torino, Italy
- INFN, Sezione di Torino, Via P. Giuria 1, 10125 Torino, Italy
| | - A Guglielmetti
- Università degli Studi di Milano, 20133 Milano, Italy
- INFN, Sezione di Milano, Via G. Celoria 16, 20133 Milano, Italy
| | - C Gustavino
- INFN, Sezione di Roma La Sapienza, Piazzale A. Moro 2, 00185 Roma, Italy
| | - Gy Gyürky
- Institute for Nuclear Research (ATOMKI), P.O. Box 51, HU-4001 Debrecen, Hungary
| | - G Imbriani
- Università di Napoli "Federico II," 80126 Napoli, Italy
- INFN, Sezione di Napoli, 80126 Napoli, Italy
| | - M Junker
- INFN, Laboratori Nazionali del Gran Sasso (LNGS), 67100 Assergi, Italy
| | - M Lugaro
- Institute of Physics, ELTE Eötvös Loránd University, 1053 Budapest, Hungary
- Konkoly Observatory, Research Centre for Astronomy and Earth Sciences, MTA Centre for Excellence, 1121 Budapest, Hungary
| | - P Marigo
- INFN, Sezione di Padova, Via F. Marzolo 8, 35131 Padova, Italy
- Università degli Studi di Padova, Via F. Marzolo 8, 35131 Padova, Italy
| | - E Masha
- Università degli Studi di Milano, 20133 Milano, Italy
- INFN, Sezione di Milano, Via G. Celoria 16, 20133 Milano, Italy
| | - R Menegazzo
- INFN, Sezione di Padova, Via F. Marzolo 8, 35131 Padova, Italy
| | - V Mossa
- INFN, Sezione di Bari, 70125 Bari, Italy
| | - F R Pantaleo
- Università degli Studi di Bari, 70121 Bari, Italy
- INFN, Sezione di Bari, 70125 Bari, Italy
| | | | - R Perrino
- INFN, Sezione di Bari, 70125 Bari, Italy
| | - D Piatti
- INFN, Sezione di Padova, Via F. Marzolo 8, 35131 Padova, Italy
- Università degli Studi di Padova, Via F. Marzolo 8, 35131 Padova, Italy
| | - P Prati
- Università degli Studi di Genova, 16126 Genova, Italy
- INFN, Sezione di Genova, Via Dodecaneso 33, 16146 Genova, Italy
| | - L Schiavulli
- Università degli Studi di Bari, 70121 Bari, Italy
- INFN, Sezione di Bari, 70125 Bari, Italy
| | - K Stöckel
- Helmholtz-Zentrum Dresden-Rossendorf, Bautzner Landstrasse 400, 01328 Dresden, Germany
- Technische Universität Dresden, Institut für Kern- und Teilchenphysik, Zellescher Weg 19, 01069 Dresden, Germany
| | - O Straniero
- INFN, Laboratori Nazionali del Gran Sasso (LNGS), 67100 Assergi, Italy
- INAF, Osservatorio Astronomico d'Abruzzo, 64100 Teramo, Italy
| | - T Szücs
- Institute for Nuclear Research (ATOMKI), P.O. Box 51, HU-4001 Debrecen, Hungary
| | - M P Takács
- Helmholtz-Zentrum Dresden-Rossendorf, Bautzner Landstrasse 400, 01328 Dresden, Germany
- Technische Universität Dresden, Institut für Kern- und Teilchenphysik, Zellescher Weg 19, 01069 Dresden, Germany
| | - F Terrasi
- INFN, Sezione di Napoli, 80126 Napoli, Italy
- Università degli Studi della Campania "L. Vanvitelli" (Caserta), 81100 Caserta, Italy
| | - D Vescovi
- INFN, Sezione of Perugia, Via A. Pascoli snc, 06123 Perugia, Italy
- Goethe University, Max-von-Laue-Strasse 1, Frankfurt am Main 60438, Germany
| | - S Zavatarelli
- INFN, Sezione di Genova, Via Dodecaneso 33, 16146 Genova, Italy
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4
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Mossa V, Stöckel K, Cavanna F, Ferraro F, Aliotta M, Barile F, Bemmerer D, Best A, Boeltzig A, Broggini C, Bruno CG, Caciolli A, Chillery T, Ciani GF, Corvisiero P, Csedreki L, Davinson T, Depalo R, Di Leva A, Elekes Z, Fiore EM, Formicola A, Fülöp Z, Gervino G, Guglielmetti A, Gustavino C, Gyürky G, Imbriani G, Junker M, Kievsky A, Kochanek I, Lugaro M, Marcucci LE, Mangano G, Marigo P, Masha E, Menegazzo R, Pantaleo FR, Paticchio V, Perrino R, Piatti D, Pisanti O, Prati P, Schiavulli L, Straniero O, Szücs T, Takács MP, Trezzi D, Viviani M, Zavatarelli S. The baryon density of the Universe from an improved rate of deuterium burning. Nature 2020; 587:210-213. [PMID: 33177669 DOI: 10.1038/s41586-020-2878-4] [Citation(s) in RCA: 58] [Impact Index Per Article: 14.5] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 05/07/2020] [Accepted: 09/16/2020] [Indexed: 11/09/2022]
Abstract
Light elements were produced in the first few minutes of the Universe through a sequence of nuclear reactions known as Big Bang nucleosynthesis (BBN)1,2. Among the light elements produced during BBN1,2, deuterium is an excellent indicator of cosmological parameters because its abundance is highly sensitive to the primordial baryon density and also depends on the number of neutrino species permeating the early Universe. Although astronomical observations of primordial deuterium abundance have reached percent accuracy3, theoretical predictions4-6 based on BBN are hampered by large uncertainties on the cross-section of the deuterium burning D(p,γ)3He reaction. Here we show that our improved cross-sections of this reaction lead to BBN estimates of the baryon density at the 1.6 percent level, in excellent agreement with a recent analysis of the cosmic microwave background7. Improved cross-section data were obtained by exploiting the negligible cosmic-ray background deep underground at the Laboratory for Underground Nuclear Astrophysics (LUNA) of the Laboratori Nazionali del Gran Sasso (Italy)8,9. We bombarded a high-purity deuterium gas target10 with an intense proton beam from the LUNA 400-kilovolt accelerator11 and detected the γ-rays from the nuclear reaction under study with a high-purity germanium detector. Our experimental results settle the most uncertain nuclear physics input to BBN calculations and substantially improve the reliability of using primordial abundances to probe the physics of the early Universe.
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Affiliation(s)
- V Mossa
- INFN, Sezione di Bari, Bari, Italy
| | - K Stöckel
- Helmholtz-Zentrum Dresden-Rossendorf, Dresden, Germany.,Technische Universität Dresden, Dresden, Germany
| | - F Cavanna
- INFN, Sezione di Genova, Genoa, Italy.,INFN, Sezione di Torino, Turin, Italy
| | - F Ferraro
- INFN, Sezione di Genova, Genoa, Italy.,Università degli Studi di Genova, Genoa, Italy
| | - M Aliotta
- School of Physics and Astronomy, SUPA, University of Edinburgh, Edinburgh, UK
| | - F Barile
- INFN, Sezione di Bari, Bari, Italy
| | - D Bemmerer
- Helmholtz-Zentrum Dresden-Rossendorf, Dresden, Germany
| | - A Best
- Università degli Studi di Napoli "Federico II", Naples, Italy.,INFN, Sezione di Napoli, Naples, Italy
| | - A Boeltzig
- Gran Sasso Science Institute, L'Aquila, Italy.,INFN, Laboratori Nazionali del Gran Sasso (LNGS), Assergi, Italy
| | | | - C G Bruno
- School of Physics and Astronomy, SUPA, University of Edinburgh, Edinburgh, UK
| | - A Caciolli
- INFN, Sezione di Padova, Padua, Italy.,Università degli Studi di Padova, Padua, Italy
| | - T Chillery
- School of Physics and Astronomy, SUPA, University of Edinburgh, Edinburgh, UK
| | - G F Ciani
- Gran Sasso Science Institute, L'Aquila, Italy.,INFN, Laboratori Nazionali del Gran Sasso (LNGS), Assergi, Italy
| | - P Corvisiero
- INFN, Sezione di Genova, Genoa, Italy.,Università degli Studi di Genova, Genoa, Italy
| | - L Csedreki
- Gran Sasso Science Institute, L'Aquila, Italy.,INFN, Laboratori Nazionali del Gran Sasso (LNGS), Assergi, Italy
| | - T Davinson
- School of Physics and Astronomy, SUPA, University of Edinburgh, Edinburgh, UK
| | - R Depalo
- INFN, Sezione di Padova, Padua, Italy
| | - A Di Leva
- Università degli Studi di Napoli "Federico II", Naples, Italy.,INFN, Sezione di Napoli, Naples, Italy
| | - Z Elekes
- Institute for Nuclear Research (Atomki), Debrecen, Hungary
| | - E M Fiore
- INFN, Sezione di Bari, Bari, Italy.,Dipartimento Interateneo di Fisica, Università degli Studi di Bari, Bari, Italy
| | - A Formicola
- INFN, Laboratori Nazionali del Gran Sasso (LNGS), Assergi, Italy
| | - Zs Fülöp
- Institute for Nuclear Research (Atomki), Debrecen, Hungary
| | - G Gervino
- Università degli Studi di Torino, Turin, Italy.,INFN, Sezione di Torino, Turin, Italy
| | - A Guglielmetti
- Università degli Studi di Milano, Milan, Italy.,INFN, Sezione di Milano, Milan, Italy
| | | | - G Gyürky
- Institute for Nuclear Research (Atomki), Debrecen, Hungary
| | - G Imbriani
- Università degli Studi di Napoli "Federico II", Naples, Italy.,INFN, Sezione di Napoli, Naples, Italy
| | - M Junker
- INFN, Laboratori Nazionali del Gran Sasso (LNGS), Assergi, Italy
| | | | - I Kochanek
- INFN, Laboratori Nazionali del Gran Sasso (LNGS), Assergi, Italy
| | - M Lugaro
- Konkoly Observatory, Research Centre for Astronomy and Earth Sciences, MTA Centre for Excellence, Budapest, Hungary.,Institute of Physics, ELTE Eötvös Loránd University, Budapest, Hungary
| | - L E Marcucci
- INFN, Sezione di Pisa, Pisa, Italy.,Dipartimento di Fisica "E. Fermi", Università degli Studi di Pisa, Pisa, Italy
| | - G Mangano
- Università degli Studi di Napoli "Federico II", Naples, Italy.,INFN, Sezione di Napoli, Naples, Italy
| | - P Marigo
- INFN, Sezione di Padova, Padua, Italy.,Università degli Studi di Padova, Padua, Italy
| | - E Masha
- Università degli Studi di Milano, Milan, Italy.,INFN, Sezione di Milano, Milan, Italy
| | | | - F R Pantaleo
- INFN, Sezione di Bari, Bari, Italy.,Dipartimento Interateneo di Fisica, Politecnico di Bari, Bari, Italy
| | | | - R Perrino
- INFN, Sezione di Bari, Bari, Italy.,INFN, Sezione di Lecce, Lecce, Italy
| | - D Piatti
- INFN, Sezione di Padova, Padua, Italy
| | - O Pisanti
- Università degli Studi di Napoli "Federico II", Naples, Italy.,INFN, Sezione di Napoli, Naples, Italy
| | - P Prati
- INFN, Sezione di Genova, Genoa, Italy.,Università degli Studi di Genova, Genoa, Italy
| | - L Schiavulli
- INFN, Sezione di Bari, Bari, Italy.,Dipartimento Interateneo di Fisica, Università degli Studi di Bari, Bari, Italy
| | - O Straniero
- INFN, Laboratori Nazionali del Gran Sasso (LNGS), Assergi, Italy.,INAF Osservatorio Astronomico d'Abruzzo, Teramo, Italy
| | - T Szücs
- Helmholtz-Zentrum Dresden-Rossendorf, Dresden, Germany
| | - M P Takács
- Helmholtz-Zentrum Dresden-Rossendorf, Dresden, Germany.,Technische Universität Dresden, Dresden, Germany
| | - D Trezzi
- Università degli Studi di Milano, Milan, Italy.,INFN, Sezione di Milano, Milan, Italy
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5
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Mohr P, Fülöp Z, Gyürky G, Kiss GG, Szücs T. Successful Prediction of Total α-Induced Reaction Cross Sections at Astrophysically Relevant Sub-Coulomb Energies Using a Novel Approach. Phys Rev Lett 2020; 124:252701. [PMID: 32639776 DOI: 10.1103/physrevlett.124.252701] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 12/19/2019] [Revised: 02/19/2020] [Accepted: 06/04/2020] [Indexed: 06/11/2023]
Abstract
The prediction of stellar (γ,α) reaction rates for heavy nuclei is based on the calculation of (α,γ) cross sections at sub-Coulomb energies. These rates are essential for modeling the nucleosynthesis of so-called p nuclei. The standard calculations in the statistical model show a dramatic sensitivity to the chosen α-nucleus potential. The present study explains the reason for this dramatic sensitivity which results from the tail of the imaginary α-nucleus potential in the underlying optical model calculation of the total reaction cross section. As an alternative to the optical model, a simple barrier transmission model is suggested. It is shown that this simple model in combination with a well-chosen α-nucleus potential is able to predict total α-induced reaction cross sections for a wide range of heavy target nuclei above A≳150 with uncertainties below a factor of 2. The new predictions from the simple model do not require any adjustment of parameters to experimental reaction cross sections whereas in previous statistical model calculations all predictions remained very uncertain because the parameters of the α-nucleus potential had to be adjusted to experimental data. The new model allows us to predict the reaction rate of the astrophysically important ^{176}W(α,γ)^{180}Os reaction with reduced uncertainties, leading to a significantly lower reaction rate at low temperatures. The new approach could also be validated for a broad range of target nuclei from A≈60 up to A≳200.
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Affiliation(s)
- P Mohr
- Institute for Nuclear Research (MTA Atomki), H-4001 Debrecen, Hungary
- Diakonie-Klinikum, D-74523 Schwäbisch Hall, Germany
| | - Zs Fülöp
- Institute for Nuclear Research (MTA Atomki), H-4001 Debrecen, Hungary
| | - Gy Gyürky
- Institute for Nuclear Research (MTA Atomki), H-4001 Debrecen, Hungary
| | - G G Kiss
- Institute for Nuclear Research (MTA Atomki), H-4001 Debrecen, Hungary
| | - T Szücs
- Institute for Nuclear Research (MTA Atomki), H-4001 Debrecen, Hungary
| |
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6
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Glorius J, Langer C, Slavkovská Z, Bott L, Brandau C, Brückner B, Blaum K, Chen X, Dababneh S, Davinson T, Erbacher P, Fiebiger S, Gaßner T, Göbel K, Groothuis M, Gumberidze A, Gyürky G, Heil M, Hess R, Hensch R, Hillmann P, Hillenbrand PM, Hinrichs O, Jurado B, Kausch T, Khodaparast A, Kisselbach T, Klapper N, Kozhuharov C, Kurtulgil D, Lane G, Lederer-Woods C, Lestinsky M, Litvinov S, Litvinov YA, Löher B, Nolden F, Petridis N, Popp U, Rauscher T, Reed M, Reifarth R, Sanjari MS, Savran D, Simon H, Spillmann U, Steck M, Stöhlker T, Stumm J, Surzhykov A, Szücs T, Nguyen TT, Taremi Zadeh A, Thomas B, Torilov SY, Törnqvist H, Träger M, Trageser C, Trotsenko S, Varga L, Volknandt M, Weick H, Weigand M, Wolf C, Woods PJ, Xing YM. Approaching the Gamow Window with Stored Ions: Direct Measurement of ^{124}Xe(p,γ) in the ESR Storage Ring. Phys Rev Lett 2019; 122:092701. [PMID: 30932526 DOI: 10.1103/physrevlett.122.092701] [Citation(s) in RCA: 3] [Impact Index Per Article: 0.6] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 12/06/2018] [Revised: 01/31/2019] [Indexed: 06/09/2023]
Abstract
We report the first measurement of low-energy proton-capture cross sections of ^{124}Xe in a heavy-ion storage ring. ^{124}Xe^{54+} ions of five different beam energies between 5.5 and 8 AMeV were stored to collide with a windowless hydrogen target. The ^{125}Cs reaction products were directly detected. The interaction energies are located on the high energy tail of the Gamow window for hot, explosive scenarios such as supernovae and x-ray binaries. The results serve as an important test of predicted astrophysical reaction rates in this mass range. Good agreement in the prediction of the astrophysically important proton width at low energy is found, with only a 30% difference between measurement and theory. Larger deviations are found above the neutron emission threshold, where also neutron and γ widths significantly impact the cross sections. The newly established experimental method is a very powerful tool to investigate nuclear reactions on rare ion beams at low center-of-mass energies.
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Affiliation(s)
- J Glorius
- GSI Helmholtzzentrum für Schwerionenforschung GmbH, Darmstadt, Germany
| | - C Langer
- Goethe Universität, Frankfurt am Main, Germany
| | | | - L Bott
- Goethe Universität, Frankfurt am Main, Germany
| | - C Brandau
- GSI Helmholtzzentrum für Schwerionenforschung GmbH, Darmstadt, Germany
- Justus-Liebig Universität, Gießen, Germany
| | - B Brückner
- Goethe Universität, Frankfurt am Main, Germany
| | - K Blaum
- Max-Planck-Institut für Kernphysik (MPIK), Heidelberg, Germany
| | - X Chen
- Institute of Modern Physics, Chinese Academy of Sciences, Lanzhou, China
| | - S Dababneh
- Al-Balqa Applied University, Salt, Jordan
| | - T Davinson
- University of Edinburgh, Edinburgh, United Kingdom
| | - P Erbacher
- Goethe Universität, Frankfurt am Main, Germany
| | - S Fiebiger
- Goethe Universität, Frankfurt am Main, Germany
| | - T Gaßner
- GSI Helmholtzzentrum für Schwerionenforschung GmbH, Darmstadt, Germany
| | - K Göbel
- Goethe Universität, Frankfurt am Main, Germany
| | - M Groothuis
- Goethe Universität, Frankfurt am Main, Germany
| | - A Gumberidze
- GSI Helmholtzzentrum für Schwerionenforschung GmbH, Darmstadt, Germany
| | - G Gyürky
- Institute for Nuclear Research (MTA Atomki), Debrecen, Hungary
| | - M Heil
- GSI Helmholtzzentrum für Schwerionenforschung GmbH, Darmstadt, Germany
| | - R Hess
- GSI Helmholtzzentrum für Schwerionenforschung GmbH, Darmstadt, Germany
| | - R Hensch
- Goethe Universität, Frankfurt am Main, Germany
| | - P Hillmann
- Goethe Universität, Frankfurt am Main, Germany
| | - P-M Hillenbrand
- GSI Helmholtzzentrum für Schwerionenforschung GmbH, Darmstadt, Germany
| | - O Hinrichs
- Goethe Universität, Frankfurt am Main, Germany
| | - B Jurado
- CENBG, CNRS-IN2P3, Gradignan, France
| | - T Kausch
- Goethe Universität, Frankfurt am Main, Germany
| | - A Khodaparast
- GSI Helmholtzzentrum für Schwerionenforschung GmbH, Darmstadt, Germany
- Goethe Universität, Frankfurt am Main, Germany
| | | | - N Klapper
- Goethe Universität, Frankfurt am Main, Germany
| | - C Kozhuharov
- GSI Helmholtzzentrum für Schwerionenforschung GmbH, Darmstadt, Germany
| | - D Kurtulgil
- Goethe Universität, Frankfurt am Main, Germany
| | - G Lane
- Australian National University, Canberra, Australia
| | | | - M Lestinsky
- GSI Helmholtzzentrum für Schwerionenforschung GmbH, Darmstadt, Germany
| | - S Litvinov
- GSI Helmholtzzentrum für Schwerionenforschung GmbH, Darmstadt, Germany
| | - Yu A Litvinov
- GSI Helmholtzzentrum für Schwerionenforschung GmbH, Darmstadt, Germany
| | - B Löher
- GSI Helmholtzzentrum für Schwerionenforschung GmbH, Darmstadt, Germany
- Technische Universität Darmstadt, Darmstadt, Germany
| | - F Nolden
- GSI Helmholtzzentrum für Schwerionenforschung GmbH, Darmstadt, Germany
| | - N Petridis
- GSI Helmholtzzentrum für Schwerionenforschung GmbH, Darmstadt, Germany
| | - U Popp
- GSI Helmholtzzentrum für Schwerionenforschung GmbH, Darmstadt, Germany
| | - T Rauscher
- Department of Physics, University of Basel, Switzerland
- Centre for Astrophysics Research, University of Hertfordshire, Hatfield, United Kingdom
| | - M Reed
- Australian National University, Canberra, Australia
| | - R Reifarth
- Goethe Universität, Frankfurt am Main, Germany
| | - M S Sanjari
- GSI Helmholtzzentrum für Schwerionenforschung GmbH, Darmstadt, Germany
| | - D Savran
- GSI Helmholtzzentrum für Schwerionenforschung GmbH, Darmstadt, Germany
| | - H Simon
- GSI Helmholtzzentrum für Schwerionenforschung GmbH, Darmstadt, Germany
| | - U Spillmann
- GSI Helmholtzzentrum für Schwerionenforschung GmbH, Darmstadt, Germany
| | - M Steck
- GSI Helmholtzzentrum für Schwerionenforschung GmbH, Darmstadt, Germany
| | - T Stöhlker
- GSI Helmholtzzentrum für Schwerionenforschung GmbH, Darmstadt, Germany
- Helmholtz-Insitut Jena, Jena, Germany
| | - J Stumm
- Goethe Universität, Frankfurt am Main, Germany
| | - A Surzhykov
- Physikalisch-Technische Bundesanstalt, Braunschweig, Germany
- Technische Universität Braunschweig, Braunschweig, Germany
| | - T Szücs
- Institute for Nuclear Research (MTA Atomki), Debrecen, Hungary
| | - T T Nguyen
- Goethe Universität, Frankfurt am Main, Germany
| | | | - B Thomas
- Goethe Universität, Frankfurt am Main, Germany
| | - S Yu Torilov
- St. Petersburg State University, St. Petersburg, Russia
| | - H Törnqvist
- GSI Helmholtzzentrum für Schwerionenforschung GmbH, Darmstadt, Germany
- Technische Universität Darmstadt, Darmstadt, Germany
| | - M Träger
- GSI Helmholtzzentrum für Schwerionenforschung GmbH, Darmstadt, Germany
| | - C Trageser
- GSI Helmholtzzentrum für Schwerionenforschung GmbH, Darmstadt, Germany
- Justus-Liebig Universität, Gießen, Germany
| | - S Trotsenko
- GSI Helmholtzzentrum für Schwerionenforschung GmbH, Darmstadt, Germany
| | - L Varga
- GSI Helmholtzzentrum für Schwerionenforschung GmbH, Darmstadt, Germany
| | - M Volknandt
- Goethe Universität, Frankfurt am Main, Germany
| | - H Weick
- GSI Helmholtzzentrum für Schwerionenforschung GmbH, Darmstadt, Germany
| | - M Weigand
- Goethe Universität, Frankfurt am Main, Germany
| | - C Wolf
- Goethe Universität, Frankfurt am Main, Germany
| | - P J Woods
- University of Edinburgh, Edinburgh, United Kingdom
| | - Y M Xing
- GSI Helmholtzzentrum für Schwerionenforschung GmbH, Darmstadt, Germany
- Institute of Modern Physics, Chinese Academy of Sciences, Lanzhou, China
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7
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Ferraro F, Takács MP, Piatti D, Cavanna F, Depalo R, Aliotta M, Bemmerer D, Best A, Boeltzig A, Broggini C, Bruno CG, Caciolli A, Chillery T, Ciani GF, Corvisiero P, Davinson T, D'Erasmo G, Di Leva A, Elekes Z, Fiore EM, Formicola A, Fülöp Z, Gervino G, Guglielmetti A, Gustavino C, Gyürky G, Imbriani G, Junker M, Karakas A, Kochanek I, Lugaro M, Marigo P, Menegazzo R, Mossa V, Pantaleo FR, Paticchio V, Perrino R, Prati P, Schiavulli L, Stöckel K, Straniero O, Szücs T, Trezzi D, Zavatarelli S. Direct Capture Cross Section and the E_{p}=71 and 105 keV Resonances in the ^{22}Ne(p,γ)^{23}Na Reaction. Phys Rev Lett 2018; 121:172701. [PMID: 30411966 DOI: 10.1103/physrevlett.121.172701] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 07/12/2018] [Revised: 09/10/2018] [Indexed: 06/08/2023]
Abstract
The ^{22}Ne(p,γ)^{23}Na reaction, part of the neon-sodium cycle of hydrogen burning, may explain the observed anticorrelation between sodium and oxygen abundances in globular cluster stars. Its rate is controlled by a number of low-energy resonances and a slowly varying nonresonant component. Three new resonances at E_{p}=156.2, 189.5, and 259.7 keV have recently been observed and confirmed. However, significant uncertainty on the reaction rate remains due to the nonresonant process and to two suggested resonances at E_{p}=71 and 105 keV. Here, new ^{22}Ne(p,γ)^{23}Na data with high statistics and low background are reported. Stringent upper limits of 6×10^{-11} and 7×10^{-11} eV (90% confidence level), respectively, are placed on the two suggested resonances. In addition, the off-resonant S factor has been measured at unprecedented low energy, constraining the contributions from a subthreshold resonance and the direct capture process. As a result, at a temperature of 0.1 GK the error bar of the ^{22}Ne(p,γ)^{23}Na rate is now reduced by 3 orders of magnitude.
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Affiliation(s)
- F Ferraro
- Università degli Studi di Genova, Via Dodecaneso 33, 16146 Genova, Italy
- Istituto Nazionale di Fisica Nucleare, Sezione di Genova, Via Dodecaneso 33, 16146 Genova, Italy
| | - M P Takács
- Helmholtz-Zentrum Dresden-Rossendorf, Bautzner Landstr. 400, 01328 Dresden, Germany
- Technische Universität Dresden, Institut für Kern- und Teilchenphysik, Zellescher Weg 19, 01069 Dresden, Germany
| | - D Piatti
- Dipartimento di Fisica e Astronomia, Università degli Studi di Padova, Via F. Marzolo 8, 35131 Padova, Italy
- Istituto Nazionale di Fisica Nucleare, Sezione di Padova, Via F. Marzolo 8, 35131 Padova, Italy
| | - F Cavanna
- Istituto Nazionale di Fisica Nucleare, Sezione di Genova, Via Dodecaneso 33, 16146 Genova, Italy
| | - R Depalo
- Dipartimento di Fisica e Astronomia, Università degli Studi di Padova, Via F. Marzolo 8, 35131 Padova, Italy
- Istituto Nazionale di Fisica Nucleare, Sezione di Padova, Via F. Marzolo 8, 35131 Padova, Italy
| | - M Aliotta
- School of Physics and Astronomy, University of Edinburgh, EH9 3FD Edinburgh, United Kingdom
| | - D Bemmerer
- Helmholtz-Zentrum Dresden-Rossendorf, Bautzner Landstr. 400, 01328 Dresden, Germany
| | - A Best
- Università degli Studi di Napoli "Federico II", Dipartimento di Fisica "E. Pancini", Via Cintia, 80126 Napoli, Italy
- Istituto Nazionale di Fisica Nucleare, Sezione di Napoli, Via Cintia, 80126 Napoli, Italy
| | - A Boeltzig
- Gran Sasso Science Institute, 67100 L'Aquila, Italy
| | - C Broggini
- Istituto Nazionale di Fisica Nucleare, Sezione di Padova, Via F. Marzolo 8, 35131 Padova, Italy
| | - C G Bruno
- School of Physics and Astronomy, University of Edinburgh, EH9 3FD Edinburgh, United Kingdom
| | - A Caciolli
- Dipartimento di Fisica e Astronomia, Università degli Studi di Padova, Via F. Marzolo 8, 35131 Padova, Italy
- Istituto Nazionale di Fisica Nucleare, Sezione di Padova, Via F. Marzolo 8, 35131 Padova, Italy
| | - T Chillery
- School of Physics and Astronomy, University of Edinburgh, EH9 3FD Edinburgh, United Kingdom
| | - G F Ciani
- Gran Sasso Science Institute, 67100 L'Aquila, Italy
- Istituto Nazionale di Fisica Nucleare Laboratori Nazionali del Gran Sasso (LNGS), 67100 Assergi (AQ), Italy
| | - P Corvisiero
- Università degli Studi di Genova, Via Dodecaneso 33, 16146 Genova, Italy
- Istituto Nazionale di Fisica Nucleare, Sezione di Genova, Via Dodecaneso 33, 16146 Genova, Italy
| | - T Davinson
- School of Physics and Astronomy, University of Edinburgh, EH9 3FD Edinburgh, United Kingdom
| | - G D'Erasmo
- Università degli Studi di Bari, 70125 Bari, Italy
- Istituto Nazionale di Fisica Nucleare, Sezione di Bari, 70125 Bari, Italy
| | - A Di Leva
- Università degli Studi di Napoli "Federico II", Dipartimento di Fisica "E. Pancini", Via Cintia, 80126 Napoli, Italy
- Istituto Nazionale di Fisica Nucleare, Sezione di Napoli, Via Cintia, 80126 Napoli, Italy
| | - Z Elekes
- Institute for Nuclear Research of the Hungarian Academy of Sciences (MTA Atomki), PO Box 51, H-4001 Debrecen, Hungary
| | - E M Fiore
- Università degli Studi di Bari, 70125 Bari, Italy
- Istituto Nazionale di Fisica Nucleare, Sezione di Bari, 70125 Bari, Italy
| | - A Formicola
- Istituto Nazionale di Fisica Nucleare Laboratori Nazionali del Gran Sasso (LNGS), 67100 Assergi (AQ), Italy
| | - Zs Fülöp
- Institute for Nuclear Research of the Hungarian Academy of Sciences (MTA Atomki), PO Box 51, H-4001 Debrecen, Hungary
| | - G Gervino
- Istituto Nazionale di Fisica Nucleare, Sezione di Torino, Via P. Giuria 1, 10125 Torino, Italy
- Università degli Studi di Torino, Via P. Giuria 1, 10125 Torino, Italy
| | - A Guglielmetti
- Università degli Studi di Milano, Via G. Celoria 16, 20133 Milano, Italy
- Istituto Nazionale di Fisica Nucleare, Sezione di Milano, Via G. Celoria 16, 20133 Milano, Italy
| | - C Gustavino
- Istituto Nazionale di Fisica Nucleare, Sezione di Roma La Sapienza, Piazzale A. Moro 2, 00185 Roma, Italy
| | - Gy Gyürky
- Institute for Nuclear Research of the Hungarian Academy of Sciences (MTA Atomki), PO Box 51, H-4001 Debrecen, Hungary
| | - G Imbriani
- Università degli Studi di Napoli "Federico II", Dipartimento di Fisica "E. Pancini", Via Cintia, 80126 Napoli, Italy
- Istituto Nazionale di Fisica Nucleare, Sezione di Napoli, Via Cintia, 80126 Napoli, Italy
| | - M Junker
- Istituto Nazionale di Fisica Nucleare Laboratori Nazionali del Gran Sasso (LNGS), 67100 Assergi (AQ), Italy
| | - A Karakas
- Monash Centre for Astrophysics, School of Physics & Astronomy, Monash University, VIC 3800, Australia
| | - I Kochanek
- Istituto Nazionale di Fisica Nucleare Laboratori Nazionali del Gran Sasso (LNGS), 67100 Assergi (AQ), Italy
| | - M Lugaro
- Konkoly Observatory, Research Centre for Astronomy and Earth Sciences, Hungarian Academy of Sciences, 1121 Budapest, Hungary
| | - P Marigo
- Dipartimento di Fisica e Astronomia, Università degli Studi di Padova, Via F. Marzolo 8, 35131 Padova, Italy
- Istituto Nazionale di Fisica Nucleare, Sezione di Padova, Via F. Marzolo 8, 35131 Padova, Italy
| | - R Menegazzo
- Istituto Nazionale di Fisica Nucleare, Sezione di Padova, Via F. Marzolo 8, 35131 Padova, Italy
| | - V Mossa
- Università degli Studi di Bari, 70125 Bari, Italy
- Istituto Nazionale di Fisica Nucleare, Sezione di Bari, 70125 Bari, Italy
| | - F R Pantaleo
- Università degli Studi di Bari, 70125 Bari, Italy
- Istituto Nazionale di Fisica Nucleare, Sezione di Bari, 70125 Bari, Italy
| | - V Paticchio
- Istituto Nazionale di Fisica Nucleare, Sezione di Bari, 70125 Bari, Italy
| | - R Perrino
- Istituto Nazionale di Fisica Nucleare, Sezione di Bari, 70125 Bari, Italy
| | - P Prati
- Università degli Studi di Genova, Via Dodecaneso 33, 16146 Genova, Italy
- Istituto Nazionale di Fisica Nucleare, Sezione di Genova, Via Dodecaneso 33, 16146 Genova, Italy
| | - L Schiavulli
- Università degli Studi di Bari, 70125 Bari, Italy
- Istituto Nazionale di Fisica Nucleare, Sezione di Bari, 70125 Bari, Italy
| | - K Stöckel
- Helmholtz-Zentrum Dresden-Rossendorf, Bautzner Landstr. 400, 01328 Dresden, Germany
- Technische Universität Dresden, Institut für Kern- und Teilchenphysik, Zellescher Weg 19, 01069 Dresden, Germany
| | - O Straniero
- Istituto Nazionale di Fisica Nucleare, Sezione di Napoli, Via Cintia, 80126 Napoli, Italy
- Osservatorio Astronomico di Collurania, 64100 Teramo, Italy
| | - T Szücs
- Helmholtz-Zentrum Dresden-Rossendorf, Bautzner Landstr. 400, 01328 Dresden, Germany
- Institute for Nuclear Research of the Hungarian Academy of Sciences (MTA Atomki), PO Box 51, H-4001 Debrecen, Hungary
| | - D Trezzi
- Università degli Studi di Milano, Via G. Celoria 16, 20133 Milano, Italy
- Istituto Nazionale di Fisica Nucleare, Sezione di Milano, Via G. Celoria 16, 20133 Milano, Italy
| | - S Zavatarelli
- Istituto Nazionale di Fisica Nucleare, Sezione di Genova, Via Dodecaneso 33, 16146 Genova, Italy
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8
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Cavanna F, Depalo R, Aliotta M, Anders M, Bemmerer D, Best A, Boeltzig A, Broggini C, Bruno CG, Caciolli A, Corvisiero P, Davinson T, di Leva A, Elekes Z, Ferraro F, Formicola A, Fülöp Z, Gervino G, Guglielmetti A, Gustavino C, Gyürky G, Imbriani G, Junker M, Menegazzo R, Mossa V, Pantaleo FR, Prati P, Scott DA, Somorjai E, Straniero O, Strieder F, Szücs T, Takács MP, Trezzi D. Erratum: Three New Low-Energy Resonances in the ^{22}Ne(p,γ)^{23}Na Reaction [Phys. Rev. Lett. 115, 252501 (2015)]. Phys Rev Lett 2018; 120:239901. [PMID: 29932705 DOI: 10.1103/physrevlett.120.239901] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.2] [Reference Citation Analysis] [What about the content of this article? (0)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 05/14/2018] [Indexed: 06/08/2023]
Abstract
This corrects the article DOI: 10.1103/PhysRevLett.115.252501.
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9
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Bruno CG, Scott DA, Aliotta M, Formicola A, Best A, Boeltzig A, Bemmerer D, Broggini C, Caciolli A, Cavanna F, Ciani GF, Corvisiero P, Davinson T, Depalo R, Di Leva A, Elekes Z, Ferraro F, Fülöp Z, Gervino G, Guglielmetti A, Gustavino C, Gyürky G, Imbriani G, Junker M, Menegazzo R, Mossa V, Pantaleo FR, Piatti D, Prati P, Somorjai E, Straniero O, Strieder F, Szücs T, Takács MP, Trezzi D. Improved Direct Measurement of the 64.5 keV Resonance Strength in the ^{17}O(p,α)^{14}N Reaction at LUNA. Phys Rev Lett 2016; 117:142502. [PMID: 27740778 DOI: 10.1103/physrevlett.117.142502] [Citation(s) in RCA: 10] [Impact Index Per Article: 1.3] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 04/29/2016] [Indexed: 06/06/2023]
Abstract
The ^{17}O(p,α)^{14}N reaction plays a key role in various astrophysical scenarios, from asymptotic giant branch stars to classical novae. It affects the synthesis of rare isotopes such as ^{17}O and ^{18}F, which can provide constraints on astrophysical models. A new direct determination of the E_{R}=64.5 keV resonance strength performed at the Laboratory for Underground Nuclear Astrophysics (LUNA) accelerator has led to the most accurate value to date ωγ=10.0±1.4_{stat}±0.7_{syst} neV, thanks to a significant background reduction underground and generally improved experimental conditions. The (bare) proton partial width of the corresponding state at E_{x}=5672 keV in ^{18}F is Γ_{p}=35±5_{stat}±3_{syst} neV. This width is about a factor of 2 higher than previously estimated, thus leading to a factor of 2 increase in the ^{17}O(p, α)^{14}N reaction rate at astrophysical temperatures relevant to shell hydrogen burning in red giant and asymptotic giant branch stars. The new rate implies lower ^{17}O/^{16}O ratios, with important implications on the interpretation of astrophysical observables from these stars.
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Affiliation(s)
- C G Bruno
- SUPA, School of Physics and Astronomy, University of Edinburgh, EH9 3FD Edinburgh, United Kingdom
| | - D A Scott
- SUPA, School of Physics and Astronomy, University of Edinburgh, EH9 3FD Edinburgh, United Kingdom
| | - M Aliotta
- SUPA, School of Physics and Astronomy, University of Edinburgh, EH9 3FD Edinburgh, United Kingdom
| | - A Formicola
- INFN, Laboratori Nazionali del Gran Sasso (LNGS), 67100 Assergi, Italy
| | - A Best
- Università di Napoli "Federico II" and INFN, Sezione di Napoli, 80126 Napoli, Italy
| | - A Boeltzig
- Gran Sasso Science Institute, INFN, Viale F. Crispi 7, 67100 L'Aquila, Italy
| | - D Bemmerer
- Helmholtz-Zentrum Dresden-Rossendorf, Bautzner Landstrasse 400, 01328 Dresden, Germany
| | - C Broggini
- INFN, Sezione di Padova, Via F. Marzolo 8, 35131 Padova, Italy
| | - A Caciolli
- Università degli Studi di Padova and INFN, Sezione di Padova, Via F. Marzolo 8, 35131 Padova, Italy
| | - F Cavanna
- Università degli Studi di Genova and INFN, Sezione di Genova, Via Dodecaneso 33, 16146 Genova, Italy
| | - G F Ciani
- Gran Sasso Science Institute, INFN, Viale F. Crispi 7, 67100 L'Aquila, Italy
| | - P Corvisiero
- Università degli Studi di Genova and INFN, Sezione di Genova, Via Dodecaneso 33, 16146 Genova, Italy
| | - T Davinson
- SUPA, School of Physics and Astronomy, University of Edinburgh, EH9 3FD Edinburgh, United Kingdom
| | - R Depalo
- Università degli Studi di Padova and INFN, Sezione di Padova, Via F. Marzolo 8, 35131 Padova, Italy
| | - A Di Leva
- Università di Napoli "Federico II" and INFN, Sezione di Napoli, 80126 Napoli, Italy
| | - Z Elekes
- Institute for Nuclear Research (MTA ATOMKI), P.O. Box 51, HU-4001 Debrecen, Hungary
| | - F Ferraro
- Università degli Studi di Genova and INFN, Sezione di Genova, Via Dodecaneso 33, 16146 Genova, Italy
| | - Zs Fülöp
- Institute for Nuclear Research (MTA ATOMKI), P.O. Box 51, HU-4001 Debrecen, Hungary
| | - G Gervino
- Università degli Studi di Torino and INFN, Sezione di Torino, Via P. Giuria 1, 10125 Torino, Italy
| | - A Guglielmetti
- Università degli Studi di Milano and INFN, Sezione di Milano, Via G. Celoria 16, 20133 Milano, Italy
| | - C Gustavino
- INFN, Sezione di Roma La Sapienza, Piazzale A. Moro 2, 00185 Roma, Italy
| | - Gy Gyürky
- Institute for Nuclear Research (MTA ATOMKI), P.O. Box 51, HU-4001 Debrecen, Hungary
| | - G Imbriani
- Università di Napoli "Federico II" and INFN, Sezione di Napoli, 80126 Napoli, Italy
| | - M Junker
- INFN, Laboratori Nazionali del Gran Sasso (LNGS), 67100 Assergi, Italy
| | - R Menegazzo
- INFN, Sezione di Padova, Via F. Marzolo 8, 35131 Padova, Italy
| | - V Mossa
- Università degli Studi di Bari e INFN, Sezione di Bari, 70125 Bari, Italy
| | - F R Pantaleo
- Università degli Studi di Bari e INFN, Sezione di Bari, 70125 Bari, Italy
| | - D Piatti
- Università degli Studi di Padova and INFN, Sezione di Padova, Via F. Marzolo 8, 35131 Padova, Italy
| | - P Prati
- Università degli Studi di Genova and INFN, Sezione di Genova, Via Dodecaneso 33, 16146 Genova, Italy
| | - E Somorjai
- Institute for Nuclear Research (MTA ATOMKI), P.O. Box 51, HU-4001 Debrecen, Hungary
| | - O Straniero
- Osservatorio Astronomico di Collurania, Teramo, INFN, Sezione di Napoli, 80126 Napoli, Italy
| | - F Strieder
- South Dakota School of Mines, 501 E. Saint Joseph Street, South Dakota 57701, USA
| | - T Szücs
- Helmholtz-Zentrum Dresden-Rossendorf, Bautzner Landstrasse 400, 01328 Dresden, Germany
| | - M P Takács
- Helmholtz-Zentrum Dresden-Rossendorf, Bautzner Landstrasse 400, 01328 Dresden, Germany
| | - D Trezzi
- Università degli Studi di Milano and INFN, Sezione di Milano, Via G. Celoria 16, 20133 Milano, Italy
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Cavanna F, Depalo R, Aliotta M, Anders M, Bemmerer D, Best A, Boeltzig A, Broggini C, Bruno CG, Caciolli A, Corvisiero P, Davinson T, di Leva A, Elekes Z, Ferraro F, Formicola A, Fülöp Z, Gervino G, Guglielmetti A, Gustavino C, Gyürky G, Imbriani G, Junker M, Menegazzo R, Mossa V, Pantaleo FR, Prati P, Scott DA, Somorjai E, Straniero O, Strieder F, Szücs T, Takács MP, Trezzi D. Three New Low-Energy Resonances in the ^{22}Ne(p,γ)^{23}Na Reaction. Phys Rev Lett 2015; 115:252501. [PMID: 26722918 DOI: 10.1103/physrevlett.115.252501] [Citation(s) in RCA: 6] [Impact Index Per Article: 0.7] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 09/17/2015] [Indexed: 06/05/2023]
Abstract
The ^{22}Ne(p,γ)^{23}Na reaction takes part in the neon-sodium cycle of hydrogen burning. This cycle affects the synthesis of the elements between ^{20}Ne and ^{27}Al in asymptotic giant branch stars and novae. The ^{22}Ne(p,γ)^{23}Na reaction rate is very uncertain because of a large number of unobserved resonances lying in the Gamow window. At proton energies below 400 keV, only upper limits exist in the literature for the resonance strengths. Previous reaction rate evaluations differ by large factors. In the present work, the first direct observations of the ^{22}Ne(p,γ)^{23}Na resonances at 156.2, 189.5, and 259.7 keV are reported. Their resonance strengths are derived with 2%-7% uncertainty. In addition, upper limits for three other resonances are greatly reduced. Data are taken using a windowless ^{22}Ne gas target and high-purity germanium detectors at the Laboratory for Underground Nuclear Astrophysics in the Gran Sasso laboratory of the National Institute for Nuclear Physics, Italy, taking advantage of the ultralow background observed deep underground. The new reaction rate is a factor of 20 higher than the recent evaluation at a temperature of 0.1 GK, relevant to nucleosynthesis in asymptotic giant branch stars.
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Affiliation(s)
- F Cavanna
- Università degli Studi di Genova and INFN, Sezione di Genova, Via Dodecaneso 33, 16146 Genova, Italy
| | - R Depalo
- Università degli Studi di Padova and INFN, Sezione di Padova, Via F. Marzolo 8, 35131 Padova, Italy
| | - M Aliotta
- SUPA, School of Physics and Astronomy, University of Edinburgh, EH9 3FD Edinburgh, United Kingdom
| | - M Anders
- Helmholtz-Zentrum Dresden-Rossendorf, Bautzner Landstr. 400, 01328 Dresden, Germany
- Technische Universität Dresden, Institut für Kern- und Teilchenphysik, Zellescher Weg 19, 01069 Dresden, Germany
| | - D Bemmerer
- Helmholtz-Zentrum Dresden-Rossendorf, Bautzner Landstr. 400, 01328 Dresden, Germany
| | - A Best
- Laboratori Nazionali del Gran Sasso (LNGS), 67100 Assergi (AQ), Italy
| | - A Boeltzig
- Gran Sasso Science Institute, 67100 LAquila, Italy
| | - C Broggini
- INFN, Sezione di Padova, Via F. Marzolo 8, 35131 Padova, Italy
| | - C G Bruno
- SUPA, School of Physics and Astronomy, University of Edinburgh, EH9 3FD Edinburgh, United Kingdom
| | - A Caciolli
- Università degli Studi di Padova and INFN, Sezione di Padova, Via F. Marzolo 8, 35131 Padova, Italy
| | - P Corvisiero
- Università degli Studi di Genova and INFN, Sezione di Genova, Via Dodecaneso 33, 16146 Genova, Italy
| | - T Davinson
- SUPA, School of Physics and Astronomy, University of Edinburgh, EH9 3JZ Edinburgh, United Kingdom
| | - A di Leva
- Università di Napoli Federico II and INFN, Sezione di Napoli, 80126 Napoli, Italy
| | - Z Elekes
- Institute for Nuclear Research (MTA ATOMKI), PO Box 51, HU-4001 Debrecen, Hungary
| | - F Ferraro
- Università degli Studi di Genova and INFN, Sezione di Genova, Via Dodecaneso 33, 16146 Genova, Italy
| | - A Formicola
- Laboratori Nazionali del Gran Sasso (LNGS), 67100 Assergi (AQ), Italy
| | - Zs Fülöp
- Institute for Nuclear Research (MTA ATOMKI), PO Box 51, HU-4001 Debrecen, Hungary
| | - G Gervino
- Università degli Studi di Torino and INFN, Sezione di Torino, Via P. Giuria 1, 10125 Torino, Italy
| | - A Guglielmetti
- Università degli Studi di Milano and INFN, Sezione di Milano, Via G. Celoria 16, 20133 Milano, Italy
| | - C Gustavino
- INFN, Sezione di Roma La Sapienza, Piazzale A. Moro 2, 00185 Roma, Italy
| | - Gy Gyürky
- Institute for Nuclear Research (MTA ATOMKI), PO Box 51, HU-4001 Debrecen, Hungary
| | - G Imbriani
- Università di Napoli Federico II and INFN, Sezione di Napoli, 80126 Napoli, Italy
| | - M Junker
- Laboratori Nazionali del Gran Sasso (LNGS), 67100 Assergi (AQ), Italy
| | - R Menegazzo
- INFN, Sezione di Padova, Via F. Marzolo 8, 35131 Padova, Italy
| | - V Mossa
- Università degli Studi di Bari and INFN, Sezione di Bari, 70125 Bari, Italy
| | - F R Pantaleo
- Università degli Studi di Bari and INFN, Sezione di Bari, 70125 Bari, Italy
| | - P Prati
- Università degli Studi di Genova and INFN, Sezione di Genova, Via Dodecaneso 33, 16146 Genova, Italy
| | - D A Scott
- SUPA, School of Physics and Astronomy, University of Edinburgh, EH9 3JZ Edinburgh, United Kingdom
| | - E Somorjai
- Institute for Nuclear Research (MTA ATOMKI), PO Box 51, HU-4001 Debrecen, Hungary
| | - O Straniero
- Osservatorio Astronomico di Collurania, Teramo, and INFN, Sezione di Napoli, Napoli, Italy
| | - F Strieder
- Institut für Experimentalphysik III, Ruhr-Universität Bochum, 44780 Bochum, Germany
| | - T Szücs
- Helmholtz-Zentrum Dresden-Rossendorf, Bautzner Landstr. 400, 01328 Dresden, Germany
| | - M P Takács
- Helmholtz-Zentrum Dresden-Rossendorf, Bautzner Landstr. 400, 01328 Dresden, Germany
- Technische Universität Dresden, Institut für Kern- und Teilchenphysik, Zellescher Weg 19, 01069 Dresden, Germany
| | - D Trezzi
- Università degli Studi di Milano and INFN, Sezione di Milano, Via G. Celoria 16, 20133 Milano, Italy
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11
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Anders M, Trezzi D, Menegazzo R, Aliotta M, Bellini A, Bemmerer D, Broggini C, Caciolli A, Corvisiero P, Costantini H, Davinson T, Elekes Z, Erhard M, Formicola A, Fülöp Z, Gervino G, Guglielmetti A, Gustavino C, Gyürky G, Junker M, Lemut A, Marta M, Mazzocchi C, Prati P, Rossi Alvarez C, Scott DA, Somorjai E, Straniero O, Szücs T. First direct measurement of the 2H(α,γ)6Li cross section at big bang energies and the primordial lithium problem. Phys Rev Lett 2014; 113:042501. [PMID: 25105610 DOI: 10.1103/physrevlett.113.042501] [Citation(s) in RCA: 14] [Impact Index Per Article: 1.4] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 01/21/2014] [Indexed: 06/03/2023]
Abstract
Recent observations of (6)Li in metal poor stars suggest a large production of this isotope during big bang nucleosynthesis (BBN). In standard BBN calculations, the (2)H(α,γ)(6)Li reaction dominates (6)Li production. This reaction has never been measured inside the BBN energy region because its cross section drops exponentially at low energy and because the electric dipole transition is strongly suppressed for the isoscalar particles (2)H and α at energies below the Coulomb barrier. Indirect measurements using the Coulomb dissociation of (6)Li only give upper limits owing to the dominance of nuclear breakup processes. Here, we report on the results of the first measurement of the (2)H(α,γ)(6)Li cross section at big bang energies. The experiment was performed deep underground at the LUNA 400 kV accelerator in Gran Sasso, Italy. The primordial (6)Li/(7)Li isotopic abundance ratio has been determined to be (1.5 ± 0.3) × 10(-5), from our experimental data and standard BBN theory. The much higher (6)Li/(7)Li values reported for halo stars will likely require a nonstandard physics explanation, as discussed in the literature.
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Affiliation(s)
- M Anders
- Helmholtz-Zentrum Dresden-Rossendorf, Bautzner Landstrasse 400, 01328 Dresden, Germany and Technische Universität Dresden, Mommsenstrasse 9, 01069 Dresden, Germany
| | - D Trezzi
- Università degli Studi di Milano and INFN, Sezione di Milano, Via G. Celoria 16, 20133 Milano, Italy
| | - R Menegazzo
- INFN, Sezione di Padova, Via F. Marzolo 8, 35131 Padova, Italy
| | - M Aliotta
- SUPA, School of Physics and Astronomy, University of Edinburgh, EH9 3JZ Edinburgh, United Kingdom
| | - A Bellini
- Università degli Studi di Genova and INFN, Sezione di Genova, Via Dodecaneso 33, 16146 Genova, Italy
| | - D Bemmerer
- Helmholtz-Zentrum Dresden-Rossendorf, Bautzner Landstrasse 400, 01328 Dresden, Germany
| | - C Broggini
- INFN, Sezione di Padova, Via F. Marzolo 8, 35131 Padova, Italy
| | - A Caciolli
- INFN, Sezione di Padova, Via F. Marzolo 8, 35131 Padova, Italy
| | - P Corvisiero
- Università degli Studi di Genova and INFN, Sezione di Genova, Via Dodecaneso 33, 16146 Genova, Italy
| | - H Costantini
- Università degli Studi di Genova and INFN, Sezione di Genova, Via Dodecaneso 33, 16146 Genova, Italy
| | - T Davinson
- SUPA, School of Physics and Astronomy, University of Edinburgh, EH9 3JZ Edinburgh, United Kingdom
| | - Z Elekes
- Helmholtz-Zentrum Dresden-Rossendorf, Bautzner Landstrasse 400, 01328 Dresden, Germany
| | - M Erhard
- INFN, Sezione di Padova, Via F. Marzolo 8, 35131 Padova, Italy
| | - A Formicola
- Laboratori Nazionali del Gran Sasso (LNGS), Via G. Acitelli 22, 67100 Assergi, Italy
| | - Zs Fülöp
- Institute of Nuclear Research (MTA ATOMKI), PO Box 51, HU-4001 Debrecen, Hungary
| | - G Gervino
- Università degli Studi di Torino and INFN, Sezione di Torino, Via P. Giuria 1, 10125 Torino, Italy
| | - A Guglielmetti
- Università degli Studi di Milano and INFN, Sezione di Milano, Via G. Celoria 16, 20133 Milano, Italy
| | - C Gustavino
- INFN, Sezione di Roma "La Sapienza", Piazzale A. Moro 2, 00185 Roma, Italy
| | - Gy Gyürky
- Institute of Nuclear Research (MTA ATOMKI), PO Box 51, HU-4001 Debrecen, Hungary
| | - M Junker
- Laboratori Nazionali del Gran Sasso (LNGS), Via G. Acitelli 22, 67100 Assergi, Italy
| | - A Lemut
- Università degli Studi di Genova and INFN, Sezione di Genova, Via Dodecaneso 33, 16146 Genova, Italy
| | - M Marta
- Helmholtz-Zentrum Dresden-Rossendorf, Bautzner Landstrasse 400, 01328 Dresden, Germany
| | - C Mazzocchi
- Università degli Studi di Milano and INFN, Sezione di Milano, Via G. Celoria 16, 20133 Milano, Italy
| | - P Prati
- Università degli Studi di Genova and INFN, Sezione di Genova, Via Dodecaneso 33, 16146 Genova, Italy
| | - C Rossi Alvarez
- INFN, Sezione di Padova, Via F. Marzolo 8, 35131 Padova, Italy
| | - D A Scott
- SUPA, School of Physics and Astronomy, University of Edinburgh, EH9 3JZ Edinburgh, United Kingdom
| | - E Somorjai
- Institute of Nuclear Research (MTA ATOMKI), PO Box 51, HU-4001 Debrecen, Hungary
| | - O Straniero
- Osservatorio Astronomico di Collurania, Via M. Maggini, 64100 Teramo, Italy and INFN, Sezione di Napoli, Via Cintia, 80126 Napoli, Italy
| | - T Szücs
- Institute of Nuclear Research (MTA ATOMKI), PO Box 51, HU-4001 Debrecen, Hungary
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Rauscher T, Dauphas N, Dillmann I, Fröhlich C, Fülöp Z, Gyürky G. Constraining the astrophysical origin of the p-nuclei through nuclear physics and meteoritic data. Rep Prog Phys 2013; 76:066201. [PMID: 23660558 DOI: 10.1088/0034-4885/76/6/066201] [Citation(s) in RCA: 15] [Impact Index Per Article: 1.4] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/02/2023]
Abstract
A small number of naturally occurring, proton-rich nuclides (the p-nuclei) cannot be made in the s- and r-processes. Their origin is not well understood. Massive stars can produce p-nuclei through photodisintegration of pre-existing intermediate and heavy nuclei. This so-called γ-process requires high stellar plasma temperatures and occurs mainly in explosive O/Ne burning during a core-collapse supernova. Although the γ-process in massive stars has been successful in producing a large range of p-nuclei, significant deficiencies remain. An increasing number of processes and sites has been studied in recent years in search of viable alternatives replacing or supplementing the massive star models. A large number of unstable nuclei, however, with only theoretically predicted reaction rates are included in the reaction network and thus the nuclear input may also bear considerable uncertainties. The current status of astrophysical models, nuclear input and observational constraints is reviewed. After an overview of currently discussed models, the focus is on the possibility to better constrain those models through different means. Meteoritic data not only provide the actual isotopic abundances of the p-nuclei but can also put constraints on the possible contribution of proton-rich nucleosynthesis. The main part of the review focuses on the nuclear uncertainties involved in the determination of the astrophysical reaction rates required for the extended reaction networks used in nucleosynthesis studies. Experimental approaches are discussed together with their necessary connection to theory, which is especially pronounced for reactions with intermediate and heavy nuclei in explosive nuclear burning, even close to stability.
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Affiliation(s)
- T Rauscher
- Department of Physics, University of Basel, 4056 Basel, Switzerland.
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13
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Scott DA, Caciolli A, Di Leva A, Formicola A, Aliotta M, Anders M, Bemmerer D, Broggini C, Campeggio M, Corvisiero P, Elekes Z, Fülöp Z, Gervino G, Guglielmetti A, Gustavino C, Gyürky G, Imbriani G, Junker M, Laubenstein M, Menegazzo R, Marta M, Napolitani E, Prati P, Rigato V, Roca V, Somorjai E, Salvo C, Straniero O, Strieder F, Szücs T, Terrasi F, Trezzi D. First direct measurement of the 17O(p,γ)18F reaction cross section at Gamow energies for classical novae. Phys Rev Lett 2012; 109:202501. [PMID: 23215474 DOI: 10.1103/physrevlett.109.202501] [Citation(s) in RCA: 8] [Impact Index Per Article: 0.7] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 09/14/2012] [Indexed: 06/01/2023]
Abstract
Classical novae are important contributors to the abundances of key isotopes, such as the radioactive (18)F, whose observation by satellite missions could provide constraints on nucleosynthesis models in novae. The (17)O(p,γ)(18)F reaction plays a critical role in the synthesis of both oxygen and fluorine isotopes, but its reaction rate is not well determined because of the lack of experimental data at energies relevant to novae explosions. In this study, the reaction cross section has been measured directly for the first time in a wide energy range E(c.m.)~/= 200-370 keV appropriate to hydrogen burning in classical novae. In addition, the E(c.m.)=183 keV resonance strength, ωγ=1.67±0.12 μeV, has been measured with the highest precision to date. The uncertainty on the (17)O(p,γ)(18)F reaction rate has been reduced by a factor of 4, thus leading to firmer constraints on accurate models of novae nucleosynthesis.
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Affiliation(s)
- D A Scott
- SUPA, School of Physics and Astronomy, University of Edinburgh, Edinburgh EH9 3JZ, United Kingdom
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14
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Gyürky G, Farkas J, Halász Z, Szücs T. Half-life measurement of 66Ga with γ-spectroscopy. Appl Radiat Isot 2011; 70:278-81. [PMID: 21868243 DOI: 10.1016/j.apradiso.2011.08.004] [Citation(s) in RCA: 6] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 04/29/2011] [Revised: 07/29/2011] [Accepted: 08/05/2011] [Indexed: 11/28/2022]
Abstract
The half-life of (66)Ga, an isotope very important for high-energy efficiency calibration of γ-detectors, has been measured using γ-spectroscopy. In order to reduce systematic uncertainties, different source production methods and γ-counting conditions have been applied. A half-life value of t(1/2)=(9.312±0.032)h has been obtained in agreement with a recent measurement but in contradiction with some of the earlier results.
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Affiliation(s)
- Gy Gyürky
- Institute of Nuclear Research (ATOMKI), H-4001 Debrecen, POB.51, Hungary.
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15
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Di Leva A, Gialanella L, Kunz R, Rogalla D, Schürmann D, Strieder F, De Cesare M, De Cesare N, D'Onofrio A, Fülöp Z, Gyürky G, Imbriani G, Mangano G, Ordine A, Roca V, Rolfs C, Romano M, Somorjai E, Terrasi F. Stellar and primordial nucleosynthesis of 7Be: measurement of 3He(alpha,gamma)7Be. Phys Rev Lett 2009; 102:232502. [PMID: 19658929 DOI: 10.1103/physrevlett.102.232502] [Citation(s) in RCA: 10] [Impact Index Per Article: 0.7] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 11/24/2008] [Revised: 02/04/2009] [Indexed: 05/28/2023]
Abstract
The 3He(alpha,gamma)7Be reaction presently represents the largest nuclear uncertainty in the predicted solar neutrino flux and has important implications on the big bang nucleosynthesis, i.e., the production of primordial 7Li. We present here the results of an experiment using the recoil separator ERNA (European Recoil separator for Nuclear Astrophysics) to detect directly the 7Be ejectiles. In addition, off-beam activation and coincidence gamma-ray measurements were performed at selected energies. At energies above 1 MeV a large discrepancy compared to previous results is observed both in the absolute value and in the energy dependence of the cross section. Based on the available data and models, a robust estimate of the cross section at the astrophysical relevant energies is proposed.
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Affiliation(s)
- A Di Leva
- INFN Sezione di Napoli, Naples, Italy
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Kiss GG, Rauscher T, Gyürky G, Simon A, Fülöp Z, Somorjai E. Coulomb suppression of the stellar enhancement factor. Phys Rev Lett 2008; 101:191101. [PMID: 19113257 DOI: 10.1103/physrevlett.101.191101] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.1] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 06/12/2008] [Revised: 08/25/2008] [Indexed: 05/27/2023]
Abstract
It is commonly assumed that reaction measurements for astrophysics should be preferably performed in the direction of a positive Q value to minimize the impact of the stellar enhancement factor, i.e., the difference between the laboratory rate and the actual stellar rate. We show that the stellar effects can be minimized in the charged particle channel, even when the reaction Q value is negative. As a demonstration, the cross section of the astrophysically relevant 85Rb(p,n)85Sr reaction has been measured by activation between 2.16 < or = Ec.m. < or = 3.96 MeV and the astrophysical reaction rate for (p, n) as well as (n, p) is directly inferred from the data. The presented arguments are also relevant for other alpha- and proton-induced reactions in the p and rp processes. Additionally, our results confirm a previously derived modification of a global optical proton potential.
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Affiliation(s)
- G G Kiss
- Institute of Nuclear Research (ATOMKI), H-4001 Debrecen, POB.51., Hungary
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17
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Tumino A, Spitaleri C, Mukhamedzhanov A, Rapisarda GG, Cherubini S, Crucillá V, Elekes Z, Fülöp Z, Gulino M, Gyürky G, Kiss G, La Cognata M, Lamia L, Mudó F, Pizzone RG, Romano S, Sergi ML, Somorjai E. Suppression of the Coulomb interaction in the off-energy-shell p - p scattering from the p + d --> p + p + n reaction. Phys Rev Lett 2007; 98:252502. [PMID: 17678018 DOI: 10.1103/physrevlett.98.252502] [Citation(s) in RCA: 7] [Impact Index Per Article: 0.4] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 01/25/2007] [Indexed: 05/16/2023]
Abstract
Off-energy-shell effects in p - p scattering have been investigated at p - p relative energies from 600 down to 80 keV applying the Trojan horse method (THM) to the p + d --> p + p + n reaction at 5 MeV. In contrast with the on-energy-shell case, no Coulomb-nuclear interference minimum has been found in the extracted THM p - p cross section, due to the suppression of the Coulomb amplitude as predicted by the half-off-energy shell calculations. This hypothesis is strengthened by the agreement between THM p - p data and calculated on-energy-shell n + n, n + p and nuclear p + p cross sections.
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Affiliation(s)
- A Tumino
- Dipartimento di Metodologie Fisiche e Chimiche per l'Ingegneria, Università di Catania, Catania, 95125 Italy
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18
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Bemmerer D, Confortola F, Costantini H, Formicola A, Gyürky G, Bonetti R, Broggini C, Corvisiero P, Elekes Z, Fülöp Z, Gervino G, Guglielmetti A, Gustavino C, Imbriani G, Junker M, Laubenstein M, Lemut A, Limata B, Lozza V, Marta M, Menegazzo R, Prati P, Roca V, Rolfs C, Alvarez CR, Somorjai E, Straniero O, Strieder F, Terrasi F, Trautvetter HP. Activation measurement of the 3He(alpha,gamma)7Be cross section at low energy. Phys Rev Lett 2006; 97:122502. [PMID: 17025958 DOI: 10.1103/physrevlett.97.122502] [Citation(s) in RCA: 12] [Impact Index Per Article: 0.7] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 07/05/2006] [Indexed: 05/12/2023]
Abstract
The nuclear physics input from the 3He(alpha,gamma)7Be cross section is a major uncertainty in the fluxes of 7Be and 8B neutrinos from the Sun predicted by solar models and in the 7Li abundance obtained in big-bang nucleosynthesis calculations. The present work reports on a new precision experiment using the activation technique at energies directly relevant to big-bang nucleosynthesis. Previously such low energies had been reached experimentally only by the prompt-gamma technique and with inferior precision. Using a windowless gas target, high beam intensity, and low background gamma-counting facilities, the 3He(alpha,gamma)7Be cross section has been determined at 127, 148, and 169 keV center-of-mass energy with a total uncertainty of 4%. The sources of systematic uncertainty are discussed in detail. The present data can be used in big-bang nucleosynthesis calculations and to constrain the extrapolation of the 3He(alpha,gamma)7Be astrophysical S factor to solar energies.
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Affiliation(s)
- D Bemmerer
- Istituto Nazionale di Fisica Nucleare (INFN), Sezione di Padova, via Marzolo 8, 35131 Padova, Italy
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