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Casanovas-Hoste A, Domingo-Pardo C, Lerendegui-Marco J, Guerrero C, Tarifeño-Saldivia A, Krtička M, Pignatari M, Calviño F, Schumann D, Heinitz S, Dressler R, Köster U, Aberle O, Andrzejewski J, Audouin L, Bécares V, Bacak M, Balibrea-Correa J, Barbagallo M, Barros S, Bečvář F, Beinrucker C, Berthoumieux E, Billowes J, Bosnar D, Brugger M, Caamaño M, Calviani M, Cano-Ott D, Cardella R, Castelluccio DM, Cerutti F, Chen YH, Chiaveri E, Colonna N, Cortés G, Cortés-Giraldo MA, Cosentino L, Damone LA, Diakaki M, Dupont E, Durán I, Fernández-Domínguez B, Ferrari A, Ferreira P, Finocchiaro P, Furman V, Göbel K, García AR, Gawlik-Ramięga A, Glodariu T, Gonçalves IF, González-Romero E, Goverdovski A, Griesmayer E, Gunsing F, Harada H, Heftrich T, Heyse J, Jenkins DG, Jericha E, Käppeler F, Kadi Y, Katabuchi T, Kavrigin P, Ketlerov V, Khryachkov V, Kimura A, Kivel N, Kokkoris M, Leal-Cidoncha E, Lederer-Woods C, Leeb H, Lo Meo S, Lonsdale SJ, Losito R, Macina D, Marganiec J, Martínez T, Massimi C, Mastinu P, Mastromarco M, Matteucci F, Maugeri EA, Mendoza E, Mengoni A, Milazzo PM, Mingrone F, Mirea M, Montesano S, Musumarra A, Nolte R, Oprea A, Patronis N, Pavlik A, Perkowski J, Porras I, Praena J, Quesada JM, Rajeev K, Rauscher T, Reifarth R, Riego-Perez A, Romanets Y, Rout PC, Rubbia C, Ryan JA, Sabaté-Gilarte M, Saxena A, Schillebeeckx P, Schmidt S, Sedyshev P, Smith AG, Stamatopoulos A, Tagliente G, Tain JL, Tassan-Got L, Tsinganis A, Valenta S, Vannini G, Variale V, Vaz P, Ventura A, Vlachoudis V, Vlastou R, Wallner A, Warren S, Weigand M, Weiss C, Wolf C, Woods PJ, Wright T, Žugec P. Shedding Light on the Origin of ^{204}Pb, the Heaviest s-Process-Only Isotope in the Solar System. PHYSICAL REVIEW LETTERS 2024; 133:052702. [PMID: 39159101 DOI: 10.1103/physrevlett.133.052702] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 07/29/2023] [Revised: 03/09/2024] [Accepted: 06/07/2024] [Indexed: 08/21/2024]
Abstract
Asymptotic giant branch stars are responsible for the production of most of the heavy isotopes beyond Sr observed in the solar system. Among them, isotopes shielded from the r-process contribution by their stable isobars are defined as s-only nuclei. For a long time the abundance of ^{204}Pb, the heaviest s-only isotope, has been a topic of debate because state-of-the-art stellar models appeared to systematically underestimate its solar abundance. Besides the impact of uncertainties from stellar models and galactic chemical evolution simulations, this discrepancy was further obscured by rather divergent theoretical estimates for the neutron capture cross section of its radioactive precursor in the neutron-capture flow, ^{204}Tl (t_{1/2}=3.78 yr), and by the lack of experimental data on this reaction. We present the first ever neutron capture measurement on ^{204}Tl, conducted at the CERN neutron time-of-flight facility n_TOF, employing a sample of only 9 mg of ^{204}Tl produced at the Institute Laue Langevin high flux reactor. By complementing our new results with semiempirical calculations we obtained, at the s-process temperatures of kT≈8 keV and kT≈30 keV, Maxwellian-averaged cross sections (MACS) of 580(168) mb and 260(90) mb, respectively. These figures are about 3% lower and 20% higher than the corresponding values widely used in astrophysical calculations, which were based only on theoretical calculations. By using the new ^{204}Tl MACS, the uncertainty arising from the ^{204}Tl(n,γ) cross section on the s-process abundance of ^{204}Pb has been reduced from ∼30% down to +8%/-6%, and the s-process calculations are in agreement with the latest solar system abundance of ^{204}Pb reported by K. Lodders in 2021.
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Affiliation(s)
| | | | | | | | | | - M Krtička
- Charles University, Prague, Czech Republic
| | - M Pignatari
- Konkoly Observatory, HUN-REN, Konkoly Thege Miklós út 15-17, H-1121 Budapest, Hungary
- MTA Centre of Excellence, Budapest, Konkoly Thege Miklós út 15-17, H-1121, Hungary
- E. A. Milne Centre for Astrophysics, University of Hull, Hull, United Kingdom
- NuGrid Collaboration 3
| | - F Calviño
- Institut de Tècniques Energètiques (INTE)-Universitat Politècnica de Catalunya, Barcelona, Spain
| | - D Schumann
- Paul Scherrer Institut (PSI), Villigen, Switzerland
| | - S Heinitz
- Paul Scherrer Institut (PSI), Villigen, Switzerland
| | - R Dressler
- Paul Scherrer Institut (PSI), Villigen, Switzerland
| | - U Köster
- Institut Laue-Langevin (ILL), Grenoble, France
| | - O Aberle
- European Organization for Nuclear Research (CERN), Switzerland
| | | | - L Audouin
- Institut de Physique Nucléaire, CNRS-IN2P3, Université Paris-Sud, Université Paris-Saclay, F-91406 Orsay Cedex, France
| | - V Bécares
- Centro de Investigaciones Energéticas Medioambientales y Tecnológicas (CIEMAT), Spain
| | - M Bacak
- TU Wien, Atominstitut, Stadionallee 2, 1020 Wien, Austria
| | - J Balibrea-Correa
- Centro de Investigaciones Energéticas Medioambientales y Tecnológicas (CIEMAT), Spain
| | - M Barbagallo
- Istituto Nazionale di Fisica Nucleare, Sezione di Bari, Bari, Italy
| | - S Barros
- Instituto Superior Técnico, Lisbon, Portugal
| | - F Bečvář
- Charles University, Prague, Czech Republic
| | | | - E Berthoumieux
- CEA Irfu, Université Paris-Saclay, F-91191 Gif-sur-Yvette, France
| | - J Billowes
- University of Manchester, Manchester, United Kingdom
| | - D Bosnar
- Department of Physics, Faculty of Science, University of Zagreb, Zagreb, Croatia
| | - M Brugger
- European Organization for Nuclear Research (CERN), Switzerland
| | - M Caamaño
- University of Santiago de Compostela, Spain
| | - M Calviani
- European Organization for Nuclear Research (CERN), Switzerland
| | - D Cano-Ott
- Centro de Investigaciones Energéticas Medioambientales y Tecnológicas (CIEMAT), Spain
| | - R Cardella
- European Organization for Nuclear Research (CERN), Switzerland
| | - D M Castelluccio
- Agenzia Nazionale per le Nuove Tecnologie (ENEA), Bologna, Italy
- Istituto Nazionale di Fisica Nucleare, Sezione di Bologna, Bologna, Italy
| | - F Cerutti
- European Organization for Nuclear Research (CERN), Switzerland
| | - Y H Chen
- Institut de Physique Nucléaire, CNRS-IN2P3, Université Paris-Sud, Université Paris-Saclay, F-91406 Orsay Cedex, France
| | - E Chiaveri
- European Organization for Nuclear Research (CERN), Switzerland
| | - N Colonna
- Istituto Nazionale di Fisica Nucleare, Sezione di Bari, Bari, Italy
| | - G Cortés
- Institut de Tècniques Energètiques (INTE)-Universitat Politècnica de Catalunya, Barcelona, Spain
| | | | - L Cosentino
- INFN Laboratori Nazionali del Sud, Catania, Italy
| | - L A Damone
- Istituto Nazionale di Fisica Nucleare, Sezione di Bari, Bari, Italy
- Dipartimento Interateneo di Fisica, Università degli Studi di Bari, Bari, Italy
| | - M Diakaki
- CEA Irfu, Université Paris-Saclay, F-91191 Gif-sur-Yvette, France
| | - E Dupont
- CEA Irfu, Université Paris-Saclay, F-91191 Gif-sur-Yvette, France
| | - I Durán
- University of Santiago de Compostela, Spain
| | | | - A Ferrari
- European Organization for Nuclear Research (CERN), Switzerland
| | - P Ferreira
- Instituto Superior Técnico, Lisbon, Portugal
| | | | - V Furman
- Affiliated with an institute (or an international laboratory) covered by a cooperation agreement with CERN
| | - K Göbel
- Goethe University Frankfurt, Frankfurt, Germany
| | - A R García
- Centro de Investigaciones Energéticas Medioambientales y Tecnológicas (CIEMAT), Spain
| | | | - T Glodariu
- Horia Hulubei National Institute of Physics and Nuclear Engineering, Romania
| | | | - E González-Romero
- Centro de Investigaciones Energéticas Medioambientales y Tecnológicas (CIEMAT), Spain
| | - A Goverdovski
- Institute of Physics and Power Engineering (IPPE), Obninsk, Russia
| | - E Griesmayer
- TU Wien, Atominstitut, Stadionallee 2, 1020 Wien, Austria
| | - F Gunsing
- European Organization for Nuclear Research (CERN), Switzerland
- CEA Irfu, Université Paris-Saclay, F-91191 Gif-sur-Yvette, France
| | - H Harada
- Japan Atomic Energy Agency (JAEA), Tokai-Mura, Japan
| | - T Heftrich
- Goethe University Frankfurt, Frankfurt, Germany
| | - J Heyse
- European Commission, Joint Research Centre (JRC), Geel, Retieseweg 111, B-2440 Geel, Belgium
| | | | - E Jericha
- TU Wien, Atominstitut, Stadionallee 2, 1020 Wien, Austria
| | - F Käppeler
- Karlsruhe Institute of Technology, Campus North, IKP, 76021 Karlsruhe, Germany
| | - Y Kadi
- European Organization for Nuclear Research (CERN), Switzerland
| | | | - P Kavrigin
- TU Wien, Atominstitut, Stadionallee 2, 1020 Wien, Austria
| | - V Ketlerov
- Institute of Physics and Power Engineering (IPPE), Obninsk, Russia
| | - V Khryachkov
- Institute of Physics and Power Engineering (IPPE), Obninsk, Russia
| | - A Kimura
- Japan Atomic Energy Agency (JAEA), Tokai-Mura, Japan
| | - N Kivel
- Paul Scherrer Institut (PSI), Villigen, Switzerland
| | - M Kokkoris
- National Technical University of Athens, Athens, Greece
| | | | - C Lederer-Woods
- School of Physics and Astronomy, University of Edinburgh, Edinburgh, United Kingdom
| | - H Leeb
- TU Wien, Atominstitut, Stadionallee 2, 1020 Wien, Austria
| | - S Lo Meo
- Agenzia Nazionale per le Nuove Tecnologie (ENEA), Bologna, Italy
- Istituto Nazionale di Fisica Nucleare, Sezione di Bologna, Bologna, Italy
| | - S J Lonsdale
- School of Physics and Astronomy, University of Edinburgh, Edinburgh, United Kingdom
| | - R Losito
- European Organization for Nuclear Research (CERN), Switzerland
| | - D Macina
- European Organization for Nuclear Research (CERN), Switzerland
| | | | - T Martínez
- Centro de Investigaciones Energéticas Medioambientales y Tecnológicas (CIEMAT), Spain
| | - C Massimi
- Istituto Nazionale di Fisica Nucleare, Sezione di Bologna, Bologna, Italy
- Dipartimento di Fisica e Astronomia, Università di Bologna, Bologna, Italy
| | - P Mastinu
- Istituto Nazionale di Fisica Nucleare, Sezione di Legnaro, Legnaro, Italy
| | - M Mastromarco
- Istituto Nazionale di Fisica Nucleare, Sezione di Bari, Bari, Italy
| | - F Matteucci
- Istituto Nazionale di Fisica Nucleare, Sezione di Trieste, Trieste, Italy
- Dipartimento di Astronomia, Università di Trieste, Trieste, Italy
| | - E A Maugeri
- Paul Scherrer Institut (PSI), Villigen, Switzerland
| | - E Mendoza
- Centro de Investigaciones Energéticas Medioambientales y Tecnológicas (CIEMAT), Spain
| | - A Mengoni
- Agenzia Nazionale per le Nuove Tecnologie (ENEA), Bologna, Italy
| | - P M Milazzo
- Istituto Nazionale di Fisica Nucleare, Sezione di Trieste, Trieste, Italy
| | - F Mingrone
- Istituto Nazionale di Fisica Nucleare, Sezione di Bologna, Bologna, Italy
| | - M Mirea
- Horia Hulubei National Institute of Physics and Nuclear Engineering, Romania
| | | | - A Musumarra
- INFN Laboratori Nazionali del Sud, Catania, Italy
- Dipartimento di Fisica e Astronomia, Università di Catania, Catania, Italy
| | - R Nolte
- Physikalisch-Technische Bundesanstalt (PTB), Bundesallee 100, 38116 Braunschweig, Germany
| | - A Oprea
- Horia Hulubei National Institute of Physics and Nuclear Engineering, Romania
| | - N Patronis
- University of Ioannina, Ioannina, Greece
| | - A Pavlik
- University of Vienna, Faculty of Physics, Vienna, Austria
| | | | - I Porras
- European Organization for Nuclear Research (CERN), Switzerland
- University of Granada, Granada, Spain
| | - J Praena
- Universidad de Sevilla, Sevilla, Spain
- University of Granada, Granada, Spain
| | | | - K Rajeev
- Bhabha Atomic Research Centre (BARC), India
| | - T Rauscher
- Centre for Astrophysics Research, University of Hertfordshire, Hatfield, United Kingdom
- Department of Physics, University of Basel, Basel, Switzerland
| | - R Reifarth
- Goethe University Frankfurt, Frankfurt, Germany
| | | | - Y Romanets
- Instituto Superior Técnico, Lisbon, Portugal
| | - P C Rout
- Bhabha Atomic Research Centre (BARC), India
| | - C Rubbia
- European Organization for Nuclear Research (CERN), Switzerland
| | - J A Ryan
- University of Manchester, Manchester, United Kingdom
| | - M Sabaté-Gilarte
- European Organization for Nuclear Research (CERN), Switzerland
- Universidad de Sevilla, Sevilla, Spain
| | - A Saxena
- Bhabha Atomic Research Centre (BARC), India
| | - P Schillebeeckx
- European Commission, Joint Research Centre (JRC), Geel, Retieseweg 111, B-2440 Geel, Belgium
| | - S Schmidt
- Goethe University Frankfurt, Frankfurt, Germany
| | - P Sedyshev
- Affiliated with an institute (or an international laboratory) covered by a cooperation agreement with CERN
| | - A G Smith
- University of Manchester, Manchester, United Kingdom
| | | | - G Tagliente
- Istituto Nazionale di Fisica Nucleare, Sezione di Bari, Bari, Italy
| | | | - L Tassan-Got
- Institut de Physique Nucléaire, CNRS-IN2P3, Université Paris-Sud, Université Paris-Saclay, F-91406 Orsay Cedex, France
| | - A Tsinganis
- National Technical University of Athens, Athens, Greece
| | - S Valenta
- Charles University, Prague, Czech Republic
| | - G Vannini
- Istituto Nazionale di Fisica Nucleare, Sezione di Bologna, Bologna, Italy
- Dipartimento di Fisica e Astronomia, Università di Bologna, Bologna, Italy
| | - V Variale
- Istituto Nazionale di Fisica Nucleare, Sezione di Bari, Bari, Italy
| | - P Vaz
- Instituto Superior Técnico, Lisbon, Portugal
| | - A Ventura
- Istituto Nazionale di Fisica Nucleare, Sezione di Bologna, Bologna, Italy
| | | | - R Vlastou
- National Technical University of Athens, Athens, Greece
| | - A Wallner
- Australian National University, Canberra, Australia
| | - S Warren
- University of Manchester, Manchester, United Kingdom
| | - M Weigand
- Goethe University Frankfurt, Frankfurt, Germany
| | - C Weiss
- European Organization for Nuclear Research (CERN), Switzerland
- TU Wien, Atominstitut, Stadionallee 2, 1020 Wien, Austria
| | - C Wolf
- Goethe University Frankfurt, Frankfurt, Germany
| | - P J Woods
- School of Physics and Astronomy, University of Edinburgh, Edinburgh, United Kingdom
| | - T Wright
- University of Manchester, Manchester, United Kingdom
| | - P Žugec
- European Organization for Nuclear Research (CERN), Switzerland
- Department of Physics, Faculty of Science, University of Zagreb, Zagreb, Croatia
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Xiong Z, Martínez-Pinedo G, Just O, Sieverding A. Production of p Nuclei from r-Process Seeds: The νr Process. PHYSICAL REVIEW LETTERS 2024; 132:192701. [PMID: 38804935 DOI: 10.1103/physrevlett.132.192701] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 05/18/2023] [Revised: 12/29/2023] [Accepted: 03/13/2024] [Indexed: 05/29/2024]
Abstract
We present a new nucleosynthesis process that may take place on neutron-rich ejecta experiencing an intensive neutrino flux. The nucleosynthesis proceeds similarly to the standard r process, a sequence of neutron captures and beta decays with, however, charged-current neutrino absorption reactions on nuclei operating much faster than beta decays. Once neutron-capture reactions freeze out the produced r process, neutron-rich nuclei undergo a fast conversion of neutrons into protons and are pushed even beyond the β stability line, producing the neutron-deficient p nuclei. This scenario, which we denote as the νr process, provides an alternative channel for the production of p nuclei and the short-lived nucleus ^{92}Nb. We discuss the necessary conditions posed on the astrophysical site for the νr process to be realized in nature. While these conditions are not fulfilled by current neutrino-hydrodynamic models of r-process sites, future models, including more complex physics and a larger variety of outflow conditions, may achieve the necessary conditions in some regions of the ejecta.
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Affiliation(s)
- Zewei Xiong
- GSI Helmholtzzentrum für Schwerionenforschung, Planckstraße 1, D-64291 Darmstadt, Germany
| | - Gabriel Martínez-Pinedo
- GSI Helmholtzzentrum für Schwerionenforschung, Planckstraße 1, D-64291 Darmstadt, Germany
- Institut für Kernphysik (Theoriezentrum), Fachbereich Physik, Technische Universität Darmstadt, Schlossgartenstraße 2, D-64289 Darmstadt, Germany
- Helmholtz Forschungsakademie Hessen für FAIR, GSI Helmholtzzentrum für Schwerionenforschung, Planckstraße 1, 64291 Darmstadt, Germany
| | - Oliver Just
- GSI Helmholtzzentrum für Schwerionenforschung, Planckstraße 1, D-64291 Darmstadt, Germany
- Astrophysical Big Bang Laboratory, RIKEN Cluster for Pioneering Research, 2-1 Hirosawa, Wako, Saitama 351-0198, Japan
| | - Andre Sieverding
- Max Planck Institute for Astrophysics, Karl-Schwarzschild-Straße 1, D-85748 Garching, Germany
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Dillmann I, Kester O, Baartman R, Chen A, Junginger T, Herwig F, Kaltchev D, Lennarz A, Planche T, Ruiz C, Vassh N. Measuring neutron capture cross sections of radioactive nuclei: From activations at the FZK Van de Graaff to direct neutron captures in inverse kinematics with a storage ring at TRIUMF. THE EUROPEAN PHYSICAL JOURNAL. A, HADRONS AND NUCLEI 2023; 59:105. [PMID: 37187510 PMCID: PMC10182137 DOI: 10.1140/epja/s10050-023-01012-9] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 12/23/2022] [Accepted: 04/13/2023] [Indexed: 05/17/2023]
Abstract
Measuring neutron capture cross sections of radioactive nuclei is a crucial step towards a better understanding of the origin of the elements heavier than iron. For decades, the precise measurement of direct neutron capture cross sections in the "stellar" energy range (eV up to a few MeV) was limited to stable and longer-lived nuclei that could be provided as physical samples and then irradiated with neutrons. New experimental methods are now being developed to extend these direct measurements towards shorter-lived radioactive nuclei (t 1 / 2 < 1 y). One project in this direction is a low-energy heavy-ion storage ring coupled to the ISAC facility at TRIUMF, Canada's accelerator laboratory in Vancouver BC, which has a compact neutron source in the ring matrix. Such a pioneering facility could be built within the next 10 years and store a wide range of radioactive ions provided directly from the existing ISOL facility, allowing for the first time to carry out direct neutron capture measurements on short-lived isotopes in inverse kinematics.
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Affiliation(s)
- Iris Dillmann
- TRIUMF, Vancouver, BC V6T 2A3 Canada
- Department of Physics and Astronomy, University of Victoria, Victoria, BC V8P 5C2 Canada
| | - Oliver Kester
- TRIUMF, Vancouver, BC V6T 2A3 Canada
- Department of Physics and Astronomy, University of Victoria, Victoria, BC V8P 5C2 Canada
| | - Richard Baartman
- TRIUMF, Vancouver, BC V6T 2A3 Canada
- Department of Physics and Astronomy, University of Victoria, Victoria, BC V8P 5C2 Canada
| | - Alan Chen
- Department of Physics and Astronomy, McMaster University, Hamilton, ON L8S 4M1 Canada
| | - Tobias Junginger
- TRIUMF, Vancouver, BC V6T 2A3 Canada
- Department of Physics and Astronomy, University of Victoria, Victoria, BC V8P 5C2 Canada
| | - Falk Herwig
- Department of Physics and Astronomy, University of Victoria, Victoria, BC V8P 5C2 Canada
| | | | - Annika Lennarz
- TRIUMF, Vancouver, BC V6T 2A3 Canada
- Department of Physics and Astronomy, McMaster University, Hamilton, ON L8S 4M1 Canada
| | - Thomas Planche
- TRIUMF, Vancouver, BC V6T 2A3 Canada
- Department of Physics and Astronomy, University of Victoria, Victoria, BC V8P 5C2 Canada
| | - Chris Ruiz
- TRIUMF, Vancouver, BC V6T 2A3 Canada
- Department of Physics and Astronomy, University of Victoria, Victoria, BC V8P 5C2 Canada
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Psaltis A, Chen AA, Longland R, Connolly DS, Brune CR, Davids B, Fallis J, Giri R, Greife U, Hutcheon DA, Kroll L, Lennarz A, Liang J, Lovely M, Luo M, Marshall C, Paneru SN, Parikh A, Ruiz C, Shotter AC, Williams M. Direct Measurement of Resonances in ^{7}Be(α,γ)^{11}C Relevant to νp-Process Nucleosynthesis. PHYSICAL REVIEW LETTERS 2022; 129:162701. [PMID: 36306775 DOI: 10.1103/physrevlett.129.162701] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 12/31/2021] [Revised: 07/01/2022] [Accepted: 08/24/2022] [Indexed: 06/16/2023]
Abstract
We have performed the first direct measurement of two resonances of the ^{7}Be(α,γ)^{11}C reaction with unknown strengths using an intense radioactive ^{7}Be beam and the DRAGON recoil separator. We report on the first measurement of the 1155 and 1110 keV resonance strengths of 1.73±0.25(stat)±0.40(syst) eV and 125_{-25}^{+27}(stat)±15(syst) meV, respectively. The present results have reduced the uncertainty in the ^{7}Be(α,γ)^{11}C reaction rate to ∼9.4%-10.7% over T=1.5-3 GK, which is relevant for nucleosynthesis in the neutrino-driven outflows of core-collapse supernovae (νp process). We find no effect of the new, constrained reaction rate on νp-process nucleosynthesis.
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Affiliation(s)
- A Psaltis
- Department of Physics and Astronomy, McMaster University, Hamilton, Ontario L8S 4M1, Canada
- The NuGrid Collaboration
| | - A A Chen
- Department of Physics and Astronomy, McMaster University, Hamilton, Ontario L8S 4M1, Canada
- The NuGrid Collaboration
| | - R Longland
- Department of Physics, North Carolina State University, Raleigh, North Carolina 27695, USA
- Triangle Universities Nuclear Laboratory, Duke University, Durham, North Carolina 27710, USA
| | - D S Connolly
- TRIUMF, 4004 Wesbrook Mall, Vancouver, British Columbia V6T 2A3, Canada
| | - C R Brune
- Department of Physics and Astronomy, Ohio University, Athens, Ohio 45701, USA
| | - B Davids
- TRIUMF, 4004 Wesbrook Mall, Vancouver, British Columbia V6T 2A3, Canada
- Department of Physics, Simon Fraser University, Burnaby, British Columbia V5A 1S6, Canada
| | - J Fallis
- North Island College, 2300 Ryan Road, Courtenay, British Columbia V9N 8N6, Canada
| | - R Giri
- Department of Physics and Astronomy, Ohio University, Athens, Ohio 45701, USA
| | - U Greife
- Department of Physics, Colorado School of Mines, Golden, Colorado 80401, USA
| | - D A Hutcheon
- TRIUMF, 4004 Wesbrook Mall, Vancouver, British Columbia V6T 2A3, Canada
| | - L Kroll
- Department of Physics and Astronomy, McMaster University, Hamilton, Ontario L8S 4M1, Canada
- The NuGrid Collaboration
| | - A Lennarz
- TRIUMF, 4004 Wesbrook Mall, Vancouver, British Columbia V6T 2A3, Canada
| | - J Liang
- Department of Physics and Astronomy, McMaster University, Hamilton, Ontario L8S 4M1, Canada
| | - M Lovely
- Department of Physics, Colorado School of Mines, Golden, Colorado 80401, USA
| | - M Luo
- Department of Physics and Astronomy, University of British Columbia, Vancouver, British Columbia V6T 1Z4, Canada
| | - C Marshall
- Department of Physics, North Carolina State University, Raleigh, North Carolina 27695, USA
- Triangle Universities Nuclear Laboratory, Duke University, Durham, North Carolina 27710, USA
| | - S N Paneru
- Department of Physics and Astronomy, Ohio University, Athens, Ohio 45701, USA
| | - A Parikh
- Department de Física, Universitat Politècnica de Catalunya, E-08036 Barcelona, Spain
| | - C Ruiz
- TRIUMF, 4004 Wesbrook Mall, Vancouver, British Columbia V6T 2A3, Canada
- Department of Physics and Astronomy, University of Victoria, Victoria, British Columbia V8W 2Y2, Canada
| | - A C Shotter
- School of Physics, University of Edinburgh EH9 3JZ Edinburgh, United Kingdom
| | - M Williams
- TRIUMF, 4004 Wesbrook Mall, Vancouver, British Columbia V6T 2A3, Canada
- Department of Physics, University of York, Heslington, York YO10 5DD, United Kingdom
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Nan W, Guo B, Chen Y, Li Z, Liu W. 22Ne(α, n)25Mg反应:大质量恒星中的关键中子源. CHINESE SCIENCE BULLETIN-CHINESE 2022. [DOI: 10.1360/tb-2022-0279] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Challenges and Requirements in High-Precision Nuclear Astrophysics Experiments. UNIVERSE 2022. [DOI: 10.3390/universe8040216] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 11/16/2022]
Abstract
In the 21th century astronomical observations, as well as astrophysical models, have become impressively precise. For a better understanding of the processes in stellar interiors, the nuclear physics of astrophysical relevance—known as nuclear astrophysics—must aim for similar precision, as such precision is not reached yet in many cases. This concerns both nuclear theory and experiment. In this paper, nuclear astrophysics experiments are put in focus. Through the example of various parameters playing a role in nuclear reaction studies, the difficulties of reaching high precision and the possible solutions are discussed.
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Heim F, Müller M, Scholz P, Wilden S, Zilges A. Cross-section measurements relevant for the astrophysical p process at the University of Cologne. EPJ WEB OF CONFERENCES 2022. [DOI: 10.1051/epjconf/202226011001] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/14/2022] Open
Abstract
The astrophysical p process unites all processes that have been introduced to explain the abundance of a group of 30 to 35 neutron-deficient nuclei which are referred to as p nuclei. In general, these p processes include large networks of nuclear reactions and a complete understanding of the individual reaction rates is required to describe the abundance of the p nuclei qualitatively and quantitatively. In many cases the involved nuclear reactions are not accessible in the laboratory, either due to their low cross sections or because they involve unstable or exotic isotopes. For those purposes, the motivation of cross-section measurements performed at the University of Cologne is twofold: First, experimentally constrained reaction rates are of direct relevance for nucleosynthesis network calculations. And second, experimental cross-section values are required to test existing theoretical descriptions and to improve their predictive power. In this work, we present the experimental setups and methods that are used to measure nuclear cross-sections at very low sensitivities and we show a detailed overview of proton-and α-induced reactions that have been measured in Cologne in the last decade.
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8
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Lotay G, Gillespie SA, Williams M, Rauscher T, Alcorta M, Amthor AM, Andreoiu CA, Baal D, Ball GC, Bhattacharjee SS, Behnamian H, Bildstein V, Burbadge C, Catford WN, Doherty DT, Esker NE, Garcia FH, Garnsworthy AB, Hackman G, Hallam S, Hudson KA, Jazrawi S, Kasanda E, Kennington ARL, Kim YH, Lennarz A, Lubna RS, Natzke CR, Nishimura N, Olaizola B, Paxman C, Psaltis A, Svensson CE, Williams J, Wallis B, Yates D, Walter D, Davids B. First Direct Measurement of an Astrophysical p-Process Reaction Cross Section Using a Radioactive Ion Beam. PHYSICAL REVIEW LETTERS 2021; 127:112701. [PMID: 34558922 DOI: 10.1103/physrevlett.127.112701] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 05/14/2021] [Revised: 07/19/2021] [Accepted: 08/11/2021] [Indexed: 06/13/2023]
Abstract
We have performed the first direct measurement of the ^{83}Rb(p,γ) radiative capture reaction cross section in inverse kinematics using a radioactive beam of ^{83}Rb at incident energies of 2.4 and 2.7A MeV. The measured cross section at an effective relative kinetic energy of E_{cm}=2.393 MeV, which lies within the relevant energy window for core collapse supernovae, is smaller than the prediction of statistical model calculations. This leads to the abundance of ^{84}Sr produced in the astrophysical p process being higher than previously calculated. Moreover, the discrepancy of the present data with theoretical predictions indicates that further experimental investigation of p-process reactions involving unstable projectiles is clearly warranted.
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Affiliation(s)
- G Lotay
- Department of Physics, University of Surrey, Guildford GU2 7XH, United Kingdom
| | - S A Gillespie
- TRIUMF, 4004 Wesbrook Mall, Vancouver, British Columbia V6T 2A3, Canada
| | - M Williams
- TRIUMF, 4004 Wesbrook Mall, Vancouver, British Columbia V6T 2A3, Canada
- Department of Physics, University of York, Heslington, York YO10 5DD, United Kingdom
| | - T Rauscher
- Department of Physics, University of Basel, Klingelbergstrasse 82, CH-4056 Basel, Switzerland
- Centre for Astrophysics Research, University of Hertfordshire, Hatfield AL10 9AB, United Kingdom
| | - M Alcorta
- TRIUMF, 4004 Wesbrook Mall, Vancouver, British Columbia V6T 2A3, Canada
| | - A M Amthor
- Department of Physics and Astronomy, Bucknell University, Lewisburg, Pennsylvania 17837, USA
| | - C A Andreoiu
- Department of Chemistry, Simon Fraser University, Burnaby, British Columbia V5A 1S6, Canada
| | - D Baal
- TRIUMF, 4004 Wesbrook Mall, Vancouver, British Columbia V6T 2A3, Canada
| | - G C Ball
- TRIUMF, 4004 Wesbrook Mall, Vancouver, British Columbia V6T 2A3, Canada
| | - S S Bhattacharjee
- TRIUMF, 4004 Wesbrook Mall, Vancouver, British Columbia V6T 2A3, Canada
| | - H Behnamian
- Department of Physics, University of Guelph, Guelph, Ontario N1G 2W1, Canada
| | - V Bildstein
- Department of Physics, University of Guelph, Guelph, Ontario N1G 2W1, Canada
| | - C Burbadge
- Department of Physics, University of Guelph, Guelph, Ontario N1G 2W1, Canada
| | - W N Catford
- Department of Physics, University of Surrey, Guildford GU2 7XH, United Kingdom
| | - D T Doherty
- Department of Physics, University of Surrey, Guildford GU2 7XH, United Kingdom
| | - N E Esker
- TRIUMF, 4004 Wesbrook Mall, Vancouver, British Columbia V6T 2A3, Canada
| | - F H Garcia
- Department of Chemistry, Simon Fraser University, Burnaby, British Columbia V5A 1S6, Canada
| | - A B Garnsworthy
- TRIUMF, 4004 Wesbrook Mall, Vancouver, British Columbia V6T 2A3, Canada
| | - G Hackman
- TRIUMF, 4004 Wesbrook Mall, Vancouver, British Columbia V6T 2A3, Canada
| | - S Hallam
- Department of Physics, University of Surrey, Guildford GU2 7XH, United Kingdom
| | - K A Hudson
- TRIUMF, 4004 Wesbrook Mall, Vancouver, British Columbia V6T 2A3, Canada
- Department of Physics, Simon Fraser University, Burnaby, British Columbia V5A 1S6, Canada
| | - S Jazrawi
- Department of Physics, University of Surrey, Guildford GU2 7XH, United Kingdom
| | - E Kasanda
- Department of Physics, University of Guelph, Guelph, Ontario N1G 2W1, Canada
| | - A R L Kennington
- Department of Physics, University of Surrey, Guildford GU2 7XH, United Kingdom
| | - Y H Kim
- Department of Nuclear Engineering, Hanyang University, Seoul 04763, Republic of Korea
| | - A Lennarz
- TRIUMF, 4004 Wesbrook Mall, Vancouver, British Columbia V6T 2A3, Canada
| | - R S Lubna
- TRIUMF, 4004 Wesbrook Mall, Vancouver, British Columbia V6T 2A3, Canada
| | - C R Natzke
- TRIUMF, 4004 Wesbrook Mall, Vancouver, British Columbia V6T 2A3, Canada
- Department of Physics, Colorado School of Mines, Golden, Colorado 80401, USA
| | - N Nishimura
- Astrophysical Big Bang Laboratory, CPR, RIKEN, Wako, Saitama 351-0198, Japan
| | - B Olaizola
- TRIUMF, 4004 Wesbrook Mall, Vancouver, British Columbia V6T 2A3, Canada
| | - C Paxman
- Department of Physics, University of Surrey, Guildford GU2 7XH, United Kingdom
- TRIUMF, 4004 Wesbrook Mall, Vancouver, British Columbia V6T 2A3, Canada
| | - A Psaltis
- Department of Physics and Astronomy, McMaster University, Hamilton, Ontario L8S 4L8, Canada
| | - C E Svensson
- Department of Physics, University of Guelph, Guelph, Ontario N1G 2W1, Canada
| | - J Williams
- TRIUMF, 4004 Wesbrook Mall, Vancouver, British Columbia V6T 2A3, Canada
| | - B Wallis
- Department of Physics, University of York, Heslington, York YO10 5DD, United Kingdom
| | - D Yates
- TRIUMF, 4004 Wesbrook Mall, Vancouver, British Columbia V6T 2A3, Canada
- Department of Physics and Astronomy, University of British Columbia, Vancouver BC V6T 1Z4, Canada
| | - D Walter
- TRIUMF, 4004 Wesbrook Mall, Vancouver, British Columbia V6T 2A3, Canada
| | - B Davids
- TRIUMF, 4004 Wesbrook Mall, Vancouver, British Columbia V6T 2A3, Canada
- Department of Physics, Simon Fraser University, Burnaby, British Columbia V5A 1S6, Canada
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Charlier BLA, Tissot FLH, Vollstaedt H, Dauphas N, Wilson CJN, Marquez RT. Survival of presolar p-nuclide carriers in the nebula revealed by stepwise leaching of Allende refractory inclusions. SCIENCE ADVANCES 2021; 7:7/28/eabf6222. [PMID: 34244141 PMCID: PMC8270483 DOI: 10.1126/sciadv.abf6222] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Download PDF] [Figures] [Subscribe] [Scholar Register] [Received: 11/08/2020] [Accepted: 05/27/2021] [Indexed: 06/13/2023]
Abstract
The 87Rb-87Sr radiochronometer provides key insights into the timing of volatile element depletion in planetary bodies, yet the unknown nucleosynthetic origin of Sr anomalies in Ca-Al-rich inclusions (CAIs, the oldest dated solar system solids) challenges the reliability of resulting chronological interpretations. To identify the nature of these Sr anomalies, we performed step-leaching experiments on nine unmelted CAIs from Allende. In six CAIs, the chemically resistant residues (0.06 to 9.7% total CAI Sr) show extreme positive μ84Sr (up to +80,655) and 87Sr variations that cannot be explained by decay of 87Rb. The extreme 84Sr but more subdued 87Sr anomalies are best explained by the presence of a presolar carrier enriched in the p-nuclide 84Sr. We argue that this unidentified carrier controls the isotopic anomalies in bulk CAIs and outer solar system materials, which reinstates the chronological significance of differences in initial 87Sr/86Sr between CAIs and volatile-depleted inner solar system materials.
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Affiliation(s)
- Bruce L A Charlier
- School of Geography, Environment and Earth Sciences, Victoria University of Wellington, Wellington 6140, New Zealand.
| | - François L H Tissot
- The Isotoparium, Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA 91125, USA
- Department of the Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA 02139, USA
| | - Hauke Vollstaedt
- Thermo Fisher Scientific, Hanna-Kunath-Str. 11, 28199 Bremen, Germany
| | - Nicolas Dauphas
- Origins Laboratory, Department of the Geophysical Sciences and Enrico Fermi Institute, The University of Chicago, 5734 South Ellis Avenue, Chicago, IL 60637, USA
| | - Colin J N Wilson
- School of Geography, Environment and Earth Sciences, Victoria University of Wellington, Wellington 6140, New Zealand
| | - Ren T Marquez
- The Isotoparium, Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA 91125, USA
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Precise initial abundance of Niobium-92 in the Solar System and implications for p-process nucleosynthesis. Proc Natl Acad Sci U S A 2021; 118:2017750118. [PMID: 33608458 DOI: 10.1073/pnas.2017750118] [Citation(s) in RCA: 7] [Impact Index Per Article: 2.3] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022] Open
Abstract
The niobium-92-zirconium-92 (92Nb-92Zr) decay system with a half-life of 37 Ma has great potential to date the evolution of planetary materials in the early Solar System. Moreover, the initial abundance of the p-process isotope 92Nb in the Solar System is important for quantifying the contribution of p-process nucleosynthesis in astrophysical models. Current estimates of the initial 92Nb/93Nb ratios have large uncertainties compromising the use of the 92Nb-92Zr cosmochronometer and leaving nucleosynthetic models poorly constrained. Here, the initial 92Nb abundance is determined to high precision by combining the 92Nb-92Zr systematics of cogenetic rutiles and zircons from mesosiderites with U-Pb dating of the same zircons. The mineral pair indicates that the 92Nb/93Nb ratio of the Solar System started with (1.66 ± 0.10) × 10-5, and their 92Zr/90Zr ratios can be explained by a three-stage Nb-Zr evolution on the mesosiderite parent body. Because of the improvement by a factor of 6 of the precision of the initial Solar System 92Nb/93Nb, we can show that the presence of 92Nb in the early Solar System provides further evidence that both type Ia supernovae and core-collapse supernovae contributed to the light p-process nuclei.
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11
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Johnson JA, Fields BD, Thompson TA. The origin of the elements: a century of progress. PHILOSOPHICAL TRANSACTIONS. SERIES A, MATHEMATICAL, PHYSICAL, AND ENGINEERING SCIENCES 2020; 378:20190301. [PMID: 32811358 DOI: 10.1098/rsta.2019.0301] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Subscribe] [Scholar Register] [Accepted: 06/02/2020] [Indexed: 06/11/2023]
Abstract
This review assesses the current state of knowledge of how the elements were produced in the Big Bang, in stellar lives and deaths, and by interactions in interstellar gas. We begin with statements of fact and discuss the evidence that convinced astronomers that the Sun is fusing hydrogen, that low-mass stars produce heavy elements through neutron capture, that massive stars can explode as supernovae and that supernovae of all types produce new elements. Nucleosynthesis in the Big Bang, through cosmic ray spallation, and in exploding white dwarfs is only ranked below the above facts in certainty because the evidence, while overwhelming, is so far circumstantial. Next, we highlight the flaws in our current understanding of the predictions for lithium production in the Big Bang and/or its destruction in stars and for the production of the elements with atomic number [Formula: see text]. While the theory that neutron star mergers produce elements through neutron-capture has powerful circumstantial evidence, we are unconvinced that they produce all of the elements past nickel. Also in dispute is the exact mechanism or mechanisms that cause the white dwarfs to explode. It is difficult to determine the origin of rare isotopes because signatures of their production are weak. We are uncertain about the production sites of some lithium and nitrogen isotopes and proton-rich heavy nuclei. Finally, Betelgeuse is probably not the next star to become a supernovae in the Milky Way, in part because Betelgeuse may collapse directly to a black hole instead. The accumulated evidence in this review shows that we understand the major production sites for the elements, but islands of uncertainty in the periodic table exist. Resolving these uncertainties requires in particular understanding explosive events with compact objects and understanding the nature of the first stars and is therefore primed for new discoveries in the next decades. This article is part of the theme issue 'Mendeleev and the periodic table'.
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Affiliation(s)
- Jennifer A Johnson
- Department of Astronomy and Center for Cosmology and AstroParticle Physics, Ohio State University, Columbus, OH 43210, USA
| | - Brian D Fields
- Departments of Astronomy and of Physics, University of Illinois, Urbana, IL 61801, USA
| | - Todd A Thompson
- Department of Astronomy and Center for Cosmology and AstroParticle Physics, Ohio State University, Columbus, OH 43210, USA
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12
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Cosmic-Ray Database Update: Ultra-High Energy, Ultra-Heavy, and Antinuclei Cosmic-Ray Data (CRDB v4.0). UNIVERSE 2020. [DOI: 10.3390/universe6080102] [Citation(s) in RCA: 16] [Impact Index Per Article: 4.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 11/16/2022]
Abstract
We present an update on CRDB, the cosmic-ray database for charged species. CRDB is based on MySQL, queried and sorted by jquery and table-sorter libraries, and displayed via PHP web pages through the AJAX protocol. We review the modifications made on the structure and outputs of the database since the first release (Maurin et al., 2014). For this update, the most important feature is the inclusion of ultra-heavy nuclei (Z>30), ultra-high energy nuclei (from 1015 to 1020 eV), and limits on antinuclei fluxes (Z≤−1 for A>1); more than 100 experiments, 350 publications, and 40,000 data points are now available in CRDB. We also revisited and simplified how users can retrieve data and submit new ones. For questions and requests, please contact crdb@lpsc.in2p3.fr.
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13
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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. PHYSICAL REVIEW LETTERS 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] [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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14
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Mitu A, Florea N, Mărginean N, Mărginean R, Căta-Danil G. Manufacturing and characterization of targets at IFIN-HH: developing an interdisciplinary body of knowledge. EPJ WEB OF CONFERENCES 2020. [DOI: 10.1051/epjconf/202022903001] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/14/2022] Open
Abstract
Target manufacturing is one fundamental issue in nuclear physics experiments using accelerators. A variety of targets are required, each having to satisfy specific conditions related to the experimental particularities. In this context, a brief description of the target preparation laboratory developed at IFIN-HH is presented in this paper. To fulfill the specific requirements, the laboratory is endowed with high performance equipment for evaporation-condensation (thermal resistance, e-based systems, sputtering) and cold rolling. During the last years, consistent technological improvements were achieved. Target characteristics, quality and reliability are important for our experiments’ feasibility in the first place, but also for the degree of confidence in the assumed accuracy. Consequently, XRD, AFM, SEM/EDX and RBS analyses are performed in collaboration with specialized departments from our institute and from other research centers.This paper is meant to synthetize our work so far.
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15
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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. PHYSICAL REVIEW LETTERS 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] [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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Cook DL, Smith T, Leya I, Hilton CD, Walker RJ, Schönbächler M. Excess 180W in IIAB iron meteorites: Identification of cosmogenic, radiogenic, and nucleosynthetic components. EARTH AND PLANETARY SCIENCE LETTERS 2018; 503:29-36. [PMID: 30846884 PMCID: PMC6398611 DOI: 10.1016/j.epsl.2018.09.021] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.2] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/09/2023]
Abstract
The origin of 180W excesses in iron meteorites has been a recently debated topic. Here, a suite of IIAB iron meteorites was studied in order to accurately determine the contribution from galactic cosmic rays (GCR) and from potential decay of 184Os to measured excesses in the minor isotope 180W. In addition to W isotopes, trace element concentrations (Re, Os, Ir, Pt, W) were determined on the same samples, as well as their cosmic ray exposure ages, using 36Cl-36Ar systematics. These data were used in combination with an improved model of GCR effects on W isotopes to correct effects resulting from neutron capture and spallation reactions. After these corrections, the residual 180W excesses correlate with Os/W ratios and indicate a clear contribution from 184Os decay. A newly derived decay constant is equivalent to a half-life for 184Os of (3.38 ± 2.13) × 1013 a. Furthermore, when the data are plotted on an Os-W isochron diagram, the intercept (ε 180Wi = 0.63 ± 0.35) reveals that the IIAB parent body was characterized by a small initial nucleosynthetic excess in 180W upon which radiogenic and GCR effects were superimposed. This is the first cogent evidence for p-process variability in W isotopes in early Solar System material.
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Affiliation(s)
- David L. Cook
- Institut für Geochemie und Petrologie, ETH Zürich, Clausiusstrasse 25, 8092 Zürich, Switzerland
| | - Thomas Smith
- Space Research and Planetology, University of Bern, Sidlerstrasse 5, 3012 Bern, Switzerland
| | - Ingo Leya
- Space Research and Planetology, University of Bern, Sidlerstrasse 5, 3012 Bern, Switzerland
| | - Connor D. Hilton
- Department of Geology, University of Maryland, 8000 Regents Dr., College Park, MD 20742, USA
| | - Richard J. Walker
- Department of Geology, University of Maryland, 8000 Regents Dr., College Park, MD 20742, USA
| | - Maria Schönbächler
- Institut für Geochemie und Petrologie, ETH Zürich, Clausiusstrasse 25, 8092 Zürich, Switzerland
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Mitu A, Oprea A, Dumitru M, Florea NM, Glodariu T, Şuvăilă R, Luculescu C, Mărginean N, Dinescu M, Căta-Danil G. Preparation and characterization of strontium targets for nuclear astrophysics experiments. J Radioanal Nucl Chem 2018. [DOI: 10.1007/s10967-018-5833-1] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.2] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 10/17/2022]
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18
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Oprea A, Glodariu T, Filipescu D, Gheorghe I, Mitu A, Boromiza M, Bucurescu D, Costache C, Cata-Danil I, Florea N, Ghita DG, Ionescu A, Marginean N, Marginean R, Mihai C, Mihai R, Negret A, Nita C, Olacel A, Pascu S, Sotty C, Suvaila R, Stan L, Stroe L, Serban A, Stiru I, Toma S, Turturica A, Ujeniuc S. Absolute cross sections of the 86Sr(α,n) 89Zr reaction at energies of astrophysical interest. EPJ WEB OF CONFERENCES 2017. [DOI: 10.1051/epjconf/201714601016] [Citation(s) in RCA: 3] [Impact Index Per Article: 0.4] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/14/2022] Open
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19
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Heim F, Mayer J, Scholz P, Spieker M, Zilges A. First results of total and partial cross-section measurements of the 107Ag(p, γ) 108Cd reaction. EPJ WEB OF CONFERENCES 2017. [DOI: 10.1051/epjconf/201716501028] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/14/2022] Open
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20
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Szücs T, Gyürky G, Halász Z, Kiss GG, Fülöp Z. α-induced reaction cross section measurements on 197Au. EPJ WEB OF CONFERENCES 2017. [DOI: 10.1051/epjconf/201716501050] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/14/2022] Open
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21
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Primitive Solar System materials and Earth share a common initial (142)Nd abundance. Nature 2016; 537:399-402. [PMID: 27629644 DOI: 10.1038/nature19351] [Citation(s) in RCA: 73] [Impact Index Per Article: 9.1] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 12/20/2015] [Accepted: 08/04/2016] [Indexed: 11/08/2022]
Abstract
The early evolution of planetesimals and planets can be constrained using variations in the abundance of neodymium-142 ((142)Nd), which arise from the initial distribution of (142)Nd within the protoplanetary disk and the radioactive decay of the short-lived samarium-146 isotope ((146)Sm). The apparent offset in (142)Nd abundance found previously between chondritic meteorites and Earth has been interpreted either as a possible consequence of nucleosynthetic variations within the protoplanetary disk or as a function of the differentiation of Earth very early in its history. Here we report high-precision Sm and Nd stable and radiogenic isotopic compositions of four calcium-aluminium-rich refractory inclusions (CAIs) from three CV-type carbonaceous chondrites, and of three whole-rock samples of unequilibrated enstatite chondrites. The CAIs, which are the first solids formed by condensation from the nebular gas, provide the best constraints for the isotopic evolution of the early Solar System. Using the mineral isochron method for individual CAIs, we find that CAIs without isotopic anomalies in Nd compared to the terrestrial composition share a (146)Sm/(144)Sm-(142)Nd/(144)Nd isotopic evolution with Earth. The average (142)Nd/(144)Nd composition for pristine enstatite chondrites that we calculate coincides with that of the accessible silicate layers of Earth. This relationship between CAIs, enstatite chondrites and Earth can only be a result of Earth having inherited the same initial abundance of (142)Nd and chondritic proportions of Sm and Nd. Consequently, (142)Nd isotopic heterogeneities found in other CAIs and among chondrite groups may arise from extrasolar grains that were present in the disk and incorporated in different proportions into these planetary objects. Our finding supports a chondritic Sm/Nd ratio for the bulk silicate Earth and, as a consequence, chondritic abundances for other refractory elements. It also removes the need for a hidden reservoir or for collisional erosion scenarios to explain the (142)Nd/(144)Nd composition of Earth.
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Tissot FLH, Dauphas N, Grossman L. Origin of uranium isotope variations in early solar nebula condensates. SCIENCE ADVANCES 2016; 2:e1501400. [PMID: 26973874 PMCID: PMC4783122 DOI: 10.1126/sciadv.1501400] [Citation(s) in RCA: 7] [Impact Index Per Article: 0.9] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 10/07/2015] [Accepted: 01/12/2016] [Indexed: 05/15/2023]
Abstract
High-temperature condensates found in meteorites display uranium isotopic variations ((235)U/(238)U), which complicate dating the solar system's formation and whose origin remains mysterious. It is possible that these variations are due to the decay of the short-lived radionuclide (247)Cm (t 1/2 = 15.6 My) into (235)U, but they could also be due to uranium kinetic isotopic fractionation during condensation. We report uranium isotope measurements of meteoritic refractory inclusions that reveal excesses of (235)U reaching ~+6% relative to average solar system composition, which can only be due to the decay of (247)Cm. This allows us to constrain the (247)Cm/(235)U ratio at solar system formation to (1.1 ± 0.3) × 10(-4). This value provides new clues on the universality of the nucleosynthetic r-process of rapid neutron capture.
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Origin of the p-process radionuclides 92Nb and 146Sm in the early solar system and inferences on the birth of the Sun. Proc Natl Acad Sci U S A 2016; 113:907-12. [PMID: 26755600 DOI: 10.1073/pnas.1519344113] [Citation(s) in RCA: 23] [Impact Index Per Article: 2.9] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022] Open
Abstract
The abundances of (92)Nb and (146)Sm in the early solar system are determined from meteoritic analysis, and their stellar production is attributed to the p process. We investigate if their origin from thermonuclear supernovae deriving from the explosion of white dwarfs with mass above the Chandrasekhar limit is in agreement with the abundance of (53)Mn, another radionuclide present in the early solar system and produced in the same events. A consistent solution for (92)Nb and (53)Mn cannot be found within the current uncertainties and requires the (92)Nb/(92)Mo ratio in the early solar system to be at least 50% lower than the current nominal value, which is outside its present error bars. A different solution is to invoke another production site for (92)Nb, which we find in the α-rich freezeout during core-collapse supernovae from massive stars. Whichever scenario we consider, we find that a relatively long time interval of at least ∼ 10 My must have elapsed from when the star-forming region where the Sun was born was isolated from the interstellar medium and the birth of the Sun. This is in agreement with results obtained from radionuclides heavier than iron produced by neutron captures and lends further support to the idea that the Sun was born in a massive star-forming region together with many thousands of stellar siblings.
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Timashev SF. Radioactive decay as a forced nuclear chemical process: Phenomenology. RUSSIAN JOURNAL OF PHYSICAL CHEMISTRY A 2015. [DOI: 10.1134/s0036024415110199] [Citation(s) in RCA: 6] [Impact Index Per Article: 0.7] [Reference Citation Analysis] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 11/23/2022]
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Rauscher T. Solution of the α-potential mystery in the γ process and its impact on the Nd/Sm ratio in meteorites. PHYSICAL REVIEW LETTERS 2013; 111:061104. [PMID: 23971552 DOI: 10.1103/physrevlett.111.061104] [Citation(s) in RCA: 3] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 05/08/2013] [Revised: 06/26/2013] [Indexed: 06/02/2023]
Abstract
The 146Sm/144Sm ratio in the early solar system has been constrained by Nd/Sm isotope ratios in meteoritic material. Predictions of 146Sm and 144Sm production in the γ process in massive stars are at odds with these constraints, and this is partly due to deficiencies in the prediction of the reaction rates involved. The production ratio depends almost exclusively on the (γ,n)/(γ,α) branching at 148Gd. A measurement of 144Sm(α,γ)148Gd at low energy had discovered considerable discrepancies between cross-section predictions and the data. Although this reaction cross section mainly depends on the optical α+nucleus potential, no global optical potential has yet been found that can consistently describe the results of this and similar α-induced reactions at the low energies encountered in astrophysical environments. The untypically large deviation in 144Sm(α,γ) and the unusual energy dependence can be explained, however, by low-energy Coulomb excitation, which is competing with compound nucleus formation at very low energies. Considering this additional reaction channel, the cross sections can be described with the usual optical potential variations, compatible with findings for (n, α) reactions in this mass range. Low-energy (α, γ) and (α, n) data on other nuclei can also be consistently explained in this way. Since Coulomb excitation does not affect α emission, the 148Gd(γ,α) rate is much higher than previously assumed. This leads to very small 146Sm/144Sm stellar production ratios, in even more pronounced conflict with the meteorite data.
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Affiliation(s)
- Thomas Rauscher
- Centre for Astrophysics Research, School of Physics, Astronomy and Mathematics, University of Hertfordshire, College Lane, Hatfield AL10 9AB, United Kingdom.
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