1
|
Tóth A, Szücs T. 3He( α, γ) 7Be cross section measurement around 7Be known energy levels. EPJ Web Conf 2022. [DOI: 10.1051/epjconf/202226011002] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/14/2022] Open
Abstract
The 3He(α,γ)7Be reaction plays an important role in two astrophysical scenarios. It is a key reaction in lithium production during the Big Bang Nucleosynthesis and one of the central reaction in the p-p chain in stars. In the case of the former event, the Gamow energy of the reaction is around 0.2 MeV, while in the case of the p-p chain in the Sun, an order of magnitude less, around 0.023 MeV. Experimental investigation at such low energies is very difficult, if possible at all, thus low energy extrapolation inevitable to predict the reaction rate at these energies. The extrapolation and its uncertainty are influenced by the precision and covered energy range of the data used. There are many precision datasets between Ec.m. = 0.3–3.1 MeV, but only one below and one above. At higher energies known levels of 7Be exist, which motivates the study of that energy range. Therefore, we performed investigations in the energy range of Ec.m. = 4.3–8.3 MeV, where the radiative cross section has not been studied so far. For the cross section determination, the activation technique was used utilising a thin-windowed gas cell and the MGC-20 cyclotron of ATOMKI.
Collapse
|
2
|
Gustavino C. Underground Nuclear Astrophysics: Present and future of the LUNA experiment. EPJ Web Conf 2019. [DOI: 10.1051/epjconf/201920901043] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/15/2022] Open
Abstract
The evolution of celestial bodies is regulated by gravitation and thermonuclear reaction rates, while the Big Bang nucleosynthesis is the result of nuclear processes in a rapidly expanding Universe. The LUNA Collaboration has shown that, by exploiting the ultra low background achievable deep underground, it is possible to study the relevant nuclear processes down to the nucleosynthesis energy inside stars and during the first minutes of Universe. In this paper the main results of LUNA are overviewed, as well as the scientific program the forthcoming 3.5 MV underground accelerator.
Collapse
|
3
|
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.
Collapse
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
| |
Collapse
|
4
|
Bemmerer D, Cowan TE, Grieger M, Hammer S, Hensel T, Junghans AR, Koppitz M, Ludwig F, Müller SE, Rimarzig B, Reinicke S, Schwengner R, Stöckel K, Szücs T, Takács MP, Turkat S, Wagner A, Wagner L, Zuber K. Felsenkeller 5 MV underground accelerator: Towards the Holy Grail of Nuclear Astrophysics 12C( α, γ) 16O. EPJ Web Conf 2018. [DOI: 10.1051/epjconf/201817801008] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [What about the content of this article? (0)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/15/2022] Open
Abstract
Low-background experiments with stable ion beams are an important tool for putting the model of stellar hydrogen, helium, and carbon burning on a solid experimental foundation. The pioneering work in this regard has been done by the LUNA collaboration at Gran Sasso, using a 0.4 MV accelerator. The present contribution reviews the status of the project for a higher-energy underground accelerator in Felsenkeller, Germany. Results from γ-ray, neutron, and muon background measurements in the Felsenkeller underground site in Dresden, Germany, show that the background conditions are satisfactory.
Two tunnels of the Felsenkeller site have recently been refurbished for the installation of a 5MV high-current Pelletron accelerator. Civil construction work has completed in March 2018. The accelerator will provide intense, 50 μA, beams of 1H+, 4He+, and 12C+ ions, enabling research on astrophysically relevant nuclear reactions with unprecedented sensitivity.
Collapse
|
5
|
Nuclear Astrophysics in underground laboratories: the LUNA experiment. EPJ Web Conf 2017. [DOI: 10.1051/epjconf/201716300009] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/14/2022] Open
|
6
|
|
7
|
|
8
|
Dohet-Eraly J, Navrátil P, Quaglioni S, Horiuchi W, Hupin G. Towards an ab initio description of light-nuclei radiative captures. EPJ Web of Conferences 2016. [DOI: 10.1051/epjconf/201611306002] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.1] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/14/2022] Open
|
9
|
Caciolli A. LUNA: Present status and future prospects. EPJ Web of Conferences 2016. [DOI: 10.1051/epjconf/201611709002] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/14/2022] Open
|
10
|
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.
Collapse
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
| |
Collapse
|
11
|
|
12
|
Bemmerer D, Cowan T, Gohl S, Ilgner C, Junghans A, Reinhardt T, Rimarzig B, Reinicke S, Röder M, Schmidt K, Schwengner R, Stöckel K, Szücs T, Takács M, Wagner A, Wagner L, Zuber K. Felsenkeller shallow-underground accelerator laboratory for nuclear astrophysics. EPJ Web of Conferences 2015. [DOI: 10.1051/epjconf/20159303010] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.1] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/15/2022] Open
|
13
|
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.
Collapse
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
| |
Collapse
|
14
|
|
15
|
|
16
|
Savin DW, Brickhouse NS, Cowan JJ, Drake RP, Federman SR, Ferland GJ, Frank A, Gudipati MS, Haxton WC, Herbst E, Profumo S, Salama F, Ziurys LM, Zweibel EG. The impact of recent advances in laboratory astrophysics on our understanding of the cosmos. Rep Prog Phys 2012; 75:036901. [PMID: 22790424 DOI: 10.1088/0034-4885/75/3/036901] [Citation(s) in RCA: 10] [Impact Index Per Article: 0.8] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/01/2023]
Abstract
An emerging theme in modern astrophysics is the connection between astronomical observations and the underlying physical phenomena that drive our cosmos. Both the mechanisms responsible for the observed astrophysical phenomena and the tools used to probe such phenomena-the radiation and particle spectra we observe-have their roots in atomic, molecular, condensed matter, plasma, nuclear and particle physics. Chemistry is implicitly included in both molecular and condensed matter physics. This connection is the theme of the present report, which provides a broad, though non-exhaustive, overview of progress in our understanding of the cosmos resulting from recent theoretical and experimental advances in what is commonly called laboratory astrophysics. This work, carried out by a diverse community of laboratory astrophysicists, is increasingly important as astrophysics transitions into an era of precise measurement and high fidelity modeling.
Collapse
Affiliation(s)
- D W Savin
- Columbia Astrophysics Laboratory, Columbia University, New York, NY 10027, USA
| | | | | | | | | | | | | | | | | | | | | | | | | | | |
Collapse
|
17
|
Neff T. Microscopic calculation of the 3He(α,γ)7Be and 3H(α,γ)7Li capture cross sections using realistic interactions. Phys Rev Lett 2011; 106:042502. [PMID: 21405326 DOI: 10.1103/physrevlett.106.042502] [Citation(s) in RCA: 7] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 11/12/2010] [Indexed: 05/30/2023]
Abstract
The radiative capture cross sections for the 3He(α,γ)7Be and 3H(α,γ)7Li reactions are calculated in the fully microscopic fermionic molecular dynamics approach using a realistic effective interaction that reproduces the nucleon-nucleon scattering data. At large distances bound and scattering states are described by antisymmetrized products of 4He and 3He/3H ground states. At short distances the many-body Hilbert space is extended with additional many-body wave functions needed to represent polarized clusters and shell-model-like configurations. Properties of the bound states are described well, as are the scattering phase shifts. The calculated S factor for the 3He(α,γ)7Be reaction agrees very well with recent experimental data in both absolute normalization and energy dependence. In the case of the 3H(α,γ)7Li reaction the calculated S factor is larger than available experimental data by about 15%.
Collapse
Affiliation(s)
- Thomas Neff
- GSI Helmholtzzentrum für Schwerionenforschung GmbH, Darmstadt, Germany.
| |
Collapse
|
18
|
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.
Collapse
Affiliation(s)
- A Di Leva
- INFN Sezione di Napoli, Naples, Italy
| | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | |
Collapse
|