First measurement of the low-energy direct capture in 20Ne(p, γ)21Na and improved energy and strength of the Ecm = 368 keV resonance

LUNA Collaboration; E. Masha; L. Barbieri; J. Skowronski; M. Aliotta; C. Ananna; F. Barile; D. Bemmerer; A. Best; A. Boeltzig; C. Broggini; C. G. Bruno; A. Caciolli; M. Campostrini; F. Cavanna; F. Casaburo; G. F. Ciani; A. Ciapponi; P. Colombetti; A. Compagnucci; P. Corvisiero; L. Csedreki; T. Davinson; R. Depalo; A. Di Leva; Z. Elekes; F. Ferraro; E. M. Fiore; A. Formicola; Zs Fülöp; G. Gervino; A. Guglielmetti; C. Gustavino; Gy Gyürky; G. Imbriani; J. José; M. Junker; M. Lugaro; P. Marigo; R. Menegazzo; P. Manoj; V. Paticchio; D. Piatti; P. Prati; D. Rapagnani; V. Rigato; D. Robb; L. Schiavulli; R. S. Sidhu; O. Straniero; T. Szücs; S. Zavatarelli

doi:10.1103/PhysRevC.108.L052801

First measurement of the low-energy direct capture in 20Ne(p, γ)21Na and improved energy and strength of the Ecm = 368 keV resonance

LUNA Collaboration, E. Masha, L. Barbieri, J. Skowronski, M. Aliotta, C. Ananna, F. Barile, D. Bemmerer, A. Best, A. Boeltzig, C. Broggini, C. G. Bruno, A. Caciolli^*, M. Campostrini, F. Cavanna, F. Casaburo, G. F. Ciani, A. Ciapponi, P. Colombetti, A. CompagnucciP. Corvisiero, L. Csedreki, T. Davinson, R. Depalo, A. Di Leva, Z. Elekes, F. Ferraro, E. M. Fiore, A. Formicola, Zs Fülöp, G. Gervino, A. Guglielmetti, C. Gustavino, Gy Gyürky, G. Imbriani, J. José, M. Junker, M. Lugaro, P. Marigo, R. Menegazzo, P. Manoj, V. Paticchio, D. Piatti, P. Prati, D. Rapagnani, V. Rigato, D. Robb, L. Schiavulli, R. S. Sidhu, O. Straniero, T. Szücs, S. Zavatarelli

^*Corresponding author for this work

School of Physics and Astronomy

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

Abstract / Description of output

The 20Ne(p, γ) 21Na reaction is the slowest in the NeNa cycle and directly affects the abundances of the Ne and Na isotopes in a variety of astrophysical sites. Here we report the measurement of its direct capture contribution, for the first time below Ecm = 352 keV, and of the contribution from the Ecm = 368 keV resonance, which dominates the reaction rate at T = 0.03−1.00 GK. The experiment was performed deep underground at the Laboratory for Underground Nuclear Astrophysics, using a high-intensity proton beam and a windowless neon gas target. Prompt γ rays from the reaction were detected with two high-purity germanium detectors. We obtain a resonance strength ωγ = (0.112± 0.002stat ± 0.005sys) meV, with an uncertainty a factor of 3 smaller than previous values. Our revised reaction rate is 20% lower than previously adopted at T < 0.1 GK and agrees with previous estimates at temperatures T ≥ 0.1 GK. Initial astrophysical implications are presented.

Original language	English
Article number	L052801
Pages (from-to)	1-7
Number of pages	7
Journal	Physical Review C
Volume	108
Issue number	5
DOIs	https://doi.org/10.1103/PhysRevC.108.L052801
Publication status	Published - 22 Nov 2023

Keywords / Materials (for Non-textual outputs)

nucl-ex
astro-ph.SR

Access to Document

10.1103/PhysRevC.108.L052801

https://arxiv.org/abs/2311.04089Licence: Creative Commons: Attribution (CC-BY)

Edinburgh Nuclear Physics Group Consolidated Grant Proposal
Woods, P., Aliotta, M., Lederer-Woods, C., Murphy, A. & Watts, D.
STFC
1/10/17 → 30/09/21
Project: Research

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LUNA Collaboration, Masha, E., Barbieri, L., Skowronski, J., Aliotta, M., Ananna, C., Barile, F., Bemmerer, D., Best, A., Boeltzig, A., Broggini, C., Bruno, C. G., Caciolli, A., Campostrini, M., Cavanna, F., Casaburo, F., Ciani, G. F., Ciapponi, A., Colombetti, P., ... Zavatarelli, S. (2023). First measurement of the low-energy direct capture in 20Ne(p, γ)21Na and improved energy and strength of the Ecm = 368 keV resonance. Physical Review C, 108(5), 1-7. Article L052801. https://doi.org/10.1103/PhysRevC.108.L052801

@article{4b466cdde8ca40178a6069eeaeb2edd1,

title = "First measurement of the low-energy direct capture in 20Ne(p, γ)21Na and improved energy and strength of the Ecm = 368 keV resonance",

abstract = "The 20Ne(p, γ) 21Na reaction is the slowest in the NeNa cycle and directly affects the abundances of the Ne and Na isotopes in a variety of astrophysical sites. Here we report the measurement of its direct capture contribution, for the first time below Ecm = 352 keV, and of the contribution from the Ecm = 368 keV resonance, which dominates the reaction rate at T = 0.03−1.00 GK. The experiment was performed deep underground at the Laboratory for Underground Nuclear Astrophysics, using a high-intensity proton beam and a windowless neon gas target. Prompt γ rays from the reaction were detected with two high-purity germanium detectors. We obtain a resonance strength ωγ = (0.112± 0.002stat ± 0.005sys) meV, with an uncertainty a factor of 3 smaller than previous values. Our revised reaction rate is 20% lower than previously adopted at T < 0.1 GK and agrees with previous estimates at temperatures T ≥ 0.1 GK. Initial astrophysical implications are presented. ",

keywords = "nucl-ex, astro-ph.SR",

author = "{LUNA Collaboration} and E. Masha and L. Barbieri and J. Skowronski and M. Aliotta and C. Ananna and F. Barile and D. Bemmerer and A. Best and A. Boeltzig and C. Broggini and Bruno, {C. G.} and A. Caciolli and M. Campostrini and F. Cavanna and F. Casaburo and Ciani, {G. F.} and A. Ciapponi and P. Colombetti and A. Compagnucci and P. Corvisiero and L. Csedreki and T. Davinson and R. Depalo and Leva, {A. Di} and Z. Elekes and F. Ferraro and Fiore, {E. M.} and A. Formicola and Zs F{\"u}l{\"o}p and G. Gervino and A. Guglielmetti and C. Gustavino and Gy Gy{\"u}rky and G. Imbriani and J. Jos{\'e} and M. Junker and M. Lugaro and P. Marigo and R. Menegazzo and P. Manoj and V. Paticchio and D. Piatti and P. Prati and D. Rapagnani and V. Rigato and D. Robb and L. Schiavulli and Sidhu, {R. S.} and O. Straniero and T. Sz{\"u}cs and S. Zavatarelli",

note = "8 pages, 4 figures, accepted to PRC (letter) Funding Information: Acknowledgments. D. Ciccotti and the technical staff of the LNGS are gratefully acknowledged for their support. We acknowledge funding from INFN, the Italian Ministry of Education, University and Research (MIUR) through the “Dipartimenti di eccellenza” project “Physics of the Universe,” the European Union (ERC-CoG STARKEY, Grant No. 615604; ERC-StG SHADES, Grant No. 852016; and ChETEC-INFRA, Grant No. 101008324), Deutsche Forschungsgemeinschaft (DFG, BE 4100-4/1), the Helmholtz Association (ERC-RA-0016), the Hungarian National Research, Development and Innovation Office (NKFIH K134197), and the European Collaboration for Science and Technology (COST Action ChETEC, CA16117). T.S. acknowledges support from the J{\'a}nos Bolyai research fellowship of the Hungarian Academy of Sciences. J.J. acknowledges support by the Spanish MINECO Grant No. PID2020-117252GB-I00 and by the AGAUR/Generalitat de Catalunya Grant No. SGR-386/2021. M.A., C.G.B., T.D., and R.S.S. acknowledge funding from STFC (Grant No. ST/P004008/1). R. J. deBoer is also gratefully acknowledged for his support in the use of the AZURE2 software for -matrix fitting. For the purpose of open access, authors have applied a Creative Commons Attribution (CC BY) licence to any Author Accepted Manuscript version arising from this submission. Publisher Copyright: {\textcopyright} 2023 American Physical Society.",

year = "2023",

month = nov,

day = "22",

doi = "10.1103/PhysRevC.108.L052801",

language = "English",

volume = "108",

pages = "1--7",

journal = "Physical Review C",

issn = "2469-9985",

publisher = "American Physical Society",

number = "5",

}

LUNA Collaboration, Masha, E, Barbieri, L, Skowronski, J, Aliotta, M, Ananna, C, Barile, F, Bemmerer, D, Best, A, Boeltzig, A, Broggini, C, Bruno, CG, Caciolli, A, Campostrini, M, Cavanna, F, Casaburo, F, Ciani, GF, Ciapponi, A, Colombetti, P, Compagnucci, A, Corvisiero, P, Csedreki, L, Davinson, T, Depalo, R, Leva, AD, Elekes, Z, Ferraro, F, Fiore, EM, Formicola, A, Fülöp, Z, Gervino, G, Guglielmetti, A, Gustavino, C, Gyürky, G, Imbriani, G, José, J, Junker, M, Lugaro, M, Marigo, P, Menegazzo, R, Manoj, P, Paticchio, V, Piatti, D, Prati, P, Rapagnani, D, Rigato, V, Robb, D, Schiavulli, L, Sidhu, RS, Straniero, O, Szücs, T & Zavatarelli, S 2023, 'First measurement of the low-energy direct capture in 20Ne(p, γ)21Na and improved energy and strength of the Ecm = 368 keV resonance', Physical Review C, vol. 108, no. 5, L052801, pp. 1-7. https://doi.org/10.1103/PhysRevC.108.L052801

TY - JOUR

T1 - First measurement of the low-energy direct capture in 20Ne(p, γ)21Na and improved energy and strength of the Ecm = 368 keV resonance

AU - LUNA Collaboration

AU - Masha, E.

AU - Barbieri, L.

AU - Skowronski, J.

AU - Aliotta, M.

AU - Ananna, C.

AU - Barile, F.

AU - Bemmerer, D.

AU - Best, A.

AU - Boeltzig, A.

AU - Broggini, C.

AU - Bruno, C. G.

AU - Caciolli, A.

AU - Campostrini, M.

AU - Cavanna, F.

AU - Casaburo, F.

AU - Ciani, G. F.

AU - Ciapponi, A.

AU - Colombetti, P.

AU - Compagnucci, A.

AU - Corvisiero, P.

AU - Csedreki, L.

AU - Davinson, T.

AU - Depalo, R.

AU - Leva, A. Di

AU - Elekes, Z.

AU - Ferraro, F.

AU - Fiore, E. M.

AU - Formicola, A.

AU - Fülöp, Zs

AU - Gervino, G.

AU - Guglielmetti, A.

AU - Gustavino, C.

AU - Gyürky, Gy

AU - Imbriani, G.

AU - José, J.

AU - Junker, M.

AU - Lugaro, M.

AU - Marigo, P.

AU - Menegazzo, R.

AU - Manoj, P.

AU - Paticchio, V.

AU - Piatti, D.

AU - Prati, P.

AU - Rapagnani, D.

AU - Rigato, V.

AU - Robb, D.

AU - Schiavulli, L.

AU - Sidhu, R. S.

AU - Straniero, O.

AU - Szücs, T.

AU - Zavatarelli, S.

N1 - 8 pages, 4 figures, accepted to PRC (letter) Funding Information: Acknowledgments. D. Ciccotti and the technical staff of the LNGS are gratefully acknowledged for their support. We acknowledge funding from INFN, the Italian Ministry of Education, University and Research (MIUR) through the “Dipartimenti di eccellenza” project “Physics of the Universe,” the European Union (ERC-CoG STARKEY, Grant No. 615604; ERC-StG SHADES, Grant No. 852016; and ChETEC-INFRA, Grant No. 101008324), Deutsche Forschungsgemeinschaft (DFG, BE 4100-4/1), the Helmholtz Association (ERC-RA-0016), the Hungarian National Research, Development and Innovation Office (NKFIH K134197), and the European Collaboration for Science and Technology (COST Action ChETEC, CA16117). T.S. acknowledges support from the János Bolyai research fellowship of the Hungarian Academy of Sciences. J.J. acknowledges support by the Spanish MINECO Grant No. PID2020-117252GB-I00 and by the AGAUR/Generalitat de Catalunya Grant No. SGR-386/2021. M.A., C.G.B., T.D., and R.S.S. acknowledge funding from STFC (Grant No. ST/P004008/1). R. J. deBoer is also gratefully acknowledged for his support in the use of the AZURE2 software for -matrix fitting. For the purpose of open access, authors have applied a Creative Commons Attribution (CC BY) licence to any Author Accepted Manuscript version arising from this submission. Publisher Copyright: © 2023 American Physical Society.

PY - 2023/11/22

Y1 - 2023/11/22

N2 - The 20Ne(p, γ) 21Na reaction is the slowest in the NeNa cycle and directly affects the abundances of the Ne and Na isotopes in a variety of astrophysical sites. Here we report the measurement of its direct capture contribution, for the first time below Ecm = 352 keV, and of the contribution from the Ecm = 368 keV resonance, which dominates the reaction rate at T = 0.03−1.00 GK. The experiment was performed deep underground at the Laboratory for Underground Nuclear Astrophysics, using a high-intensity proton beam and a windowless neon gas target. Prompt γ rays from the reaction were detected with two high-purity germanium detectors. We obtain a resonance strength ωγ = (0.112± 0.002stat ± 0.005sys) meV, with an uncertainty a factor of 3 smaller than previous values. Our revised reaction rate is 20% lower than previously adopted at T < 0.1 GK and agrees with previous estimates at temperatures T ≥ 0.1 GK. Initial astrophysical implications are presented.

AB - The 20Ne(p, γ) 21Na reaction is the slowest in the NeNa cycle and directly affects the abundances of the Ne and Na isotopes in a variety of astrophysical sites. Here we report the measurement of its direct capture contribution, for the first time below Ecm = 352 keV, and of the contribution from the Ecm = 368 keV resonance, which dominates the reaction rate at T = 0.03−1.00 GK. The experiment was performed deep underground at the Laboratory for Underground Nuclear Astrophysics, using a high-intensity proton beam and a windowless neon gas target. Prompt γ rays from the reaction were detected with two high-purity germanium detectors. We obtain a resonance strength ωγ = (0.112± 0.002stat ± 0.005sys) meV, with an uncertainty a factor of 3 smaller than previous values. Our revised reaction rate is 20% lower than previously adopted at T < 0.1 GK and agrees with previous estimates at temperatures T ≥ 0.1 GK. Initial astrophysical implications are presented.

KW - nucl-ex

KW - astro-ph.SR

U2 - 10.1103/PhysRevC.108.L052801

DO - 10.1103/PhysRevC.108.L052801

M3 - Article

SN - 2469-9985

VL - 108

SP - 1

EP - 7

JO - Physical Review C

JF - Physical Review C

IS - 5

M1 - L052801

ER -

First measurement of the low-energy direct capture in 20Ne(p, γ)21Na and improved energy and strength of the Ecm = 368 keV resonance

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Keywords / Materials (for Non-textual outputs)

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Edinburgh Nuclear Physics Group Consolidated Grant Proposal

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