First direct measurement of the 64.5 keV resonance strength in the 17O(𝑝,𝛾)18F reaction

LUNA Collaboration; R M Gesue; G F  Ciani; D Piatti; A Boeltzig; D. Rapagnani; M. Aliotta; C. Ananna; L. Barbieri; F Barile; D Bemmerer; A Best; C Broggini; C. G. Bruno; A Caciolli; M. Campostrini; F. Casaburo; F Cavanna; P Colombetti; A. Compagnucci; P Corvisiero; L. Csedreki; T. Davinson; G.M. De Gregorio; D. Dell' Aquila; R Depalo; A  Di Leva; Z Elekes; F Ferraro; A Formicola; Zs Fulop; G Gervino; A Guglielmetti; C Gustavino; Gy Gyurky; G Imbriani; M Junker; M Lugaro; P Marigo; J. Marsh; E Masha; R Menegazzo; D Mercogliano; V Paticchio; R Perrino; P Prati; V. Rigato; D. Robb; L Schiavulli; R.S. Sidhu; J. Skowronski; O Straniero; T Szucs; S Zavatarelli

doi:10.1103/PhysRevLett.133.052701

First direct measurement of the 64.5 keV resonance strength in the 17O(𝑝,𝛾)18F reaction

LUNA Collaboration, R M Gesue, G F Ciani^*, D Piatti^*, A Boeltzig, D. Rapagnani, M. Aliotta, C. Ananna, L. Barbieri, F Barile, D Bemmerer, A Best, C Broggini, C. G. Bruno, A Caciolli, M. Campostrini, F. Casaburo, F Cavanna, P Colombetti, A. CompagnucciP Corvisiero, L. Csedreki, T. Davinson, G.M. De Gregorio, D. Dell' Aquila, R Depalo, A Di Leva, Z Elekes, F Ferraro, A Formicola, Zs Fulop, G Gervino, A Guglielmetti, C Gustavino, Gy Gyurky, G Imbriani, M Junker, M Lugaro, P Marigo, J. Marsh, E Masha, R Menegazzo, D Mercogliano, V Paticchio, R Perrino, P Prati, V. Rigato, D. Robb, L Schiavulli, R.S. Sidhu, J. Skowronski, O Straniero, T Szucs, 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 CNO cycle is one of the most important nuclear energy sources in stars. At temperatures
of hydrostatic H-burning (20 MK < T < 80 MK) the 17O(p,γ) 18F reaction rate is dominated by
the poorly constrained 64.5 keV resonance. Here we report on the first direct measurements of its resonance strength and of the direct capture contribution at 142 keV, performed with a new high sensitivity setup at LUNA. The present resonance strength of ωγ(p,γ) bare = (30 ± 6stat ± 2syst) peV is about a factor of 2 higher than the values in literature, leading to a Γp bare = (34 ± 7stat ±
3syst) neV, in agreement with LUNA result from the (p,α) channel. Such agreement strengthen
our understanding of the oxygen isotopic ratios measured in red giant stars and in O-rich presolar grains.

Original language	English
Article number	052701
Pages (from-to)	1-6
Number of pages	6
Journal	Physical Review Letters
Volume	133
Issue number	5
Early online date	30 Jul 2024
DOIs	https://doi.org/10.1103/PhysRevLett.133.052701
Publication status	Published - 2 Aug 2024

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10.1103/PhysRevLett.133.052701

LQ1887220Accepted author manuscript, 432 KBLicence: Creative Commons: Attribution (CC-BY)

Edinburgh Nuclear Physics Group Consolidated Grant Proposal
Woods, P., Aliotta, M., Murphy, A. & Watts, D.
STFC
1/08/14 → 30/09/18
Project: Research

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LUNA Collaboration, Gesue, R. M., Ciani, G. F., Piatti, D., Boeltzig, A., Rapagnani, D., Aliotta, M., Ananna, C., Barbieri, L., Barile, F., Bemmerer, D., Best, A., Broggini, C., Bruno, C. G., Caciolli, A., Campostrini, M., Casaburo, F., Cavanna, F., Colombetti, P., ... Zavatarelli, S. (2024). First direct measurement of the 64.5 keV resonance strength in the 17O(𝑝,𝛾)18F reaction. Physical Review Letters, 133(5), 1-6. Article 052701. https://doi.org/10.1103/PhysRevLett.133.052701

@article{a0470c865bc84c9382dd2256dfa242a7,

title = "First direct measurement of the 64.5 keV resonance strength in the 17O(𝑝,𝛾)18F reaction",

abstract = "The CNO cycle is one of the most important nuclear energy sources in stars. At temperaturesof hydrostatic H-burning (20 MK < T < 80 MK) the 17O(p,γ) 18F reaction rate is dominated bythe poorly constrained 64.5 keV resonance. Here we report on the first direct measurements of its resonance strength and of the direct capture contribution at 142 keV, performed with a new high sensitivity setup at LUNA. The present resonance strength of ωγ(p,γ) bare = (30 ± 6stat ± 2syst) peV is about a factor of 2 higher than the values in literature, leading to a Γp bare = (34 ± 7stat ±3syst) neV, in agreement with LUNA result from the (p,α) channel. Such agreement strengthenour understanding of the oxygen isotopic ratios measured in red giant stars and in O-rich presolar grains.",

author = "{LUNA Collaboration} and Gesue, {R M} and Ciani, {G F} and D Piatti and A Boeltzig and D. Rapagnani and M. Aliotta and C. Ananna and L. Barbieri and F Barile and D Bemmerer and A Best and C Broggini and Bruno, {C. G.} and A Caciolli and M. Campostrini and F. Casaburo and F Cavanna and P Colombetti and A. Compagnucci and P Corvisiero and L. Csedreki and T. Davinson and {De Gregorio}, G.M. and {Dell' Aquila}, D. and R Depalo and {Di Leva}, A and Z Elekes and F Ferraro and A Formicola and Zs Fulop and G Gervino and A Guglielmetti and C Gustavino and Gy Gyurky and G Imbriani and M Junker and M Lugaro and P Marigo and J. Marsh and E Masha and R Menegazzo and D Mercogliano and V Paticchio and R Perrino and P Prati and V. Rigato and D. Robb and L Schiavulli and R.S. Sidhu and J. Skowronski and O Straniero and T Szucs and S Zavatarelli",

year = "2024",

month = aug,

day = "2",

doi = "10.1103/PhysRevLett.133.052701",

language = "English",

volume = "133",

pages = "1--6",

journal = "Physical Review Letters",

issn = "0031-9007",

publisher = "American Physical Society",

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}

LUNA Collaboration, Gesue, RM, Ciani, GF, Piatti, D, Boeltzig, A, Rapagnani, D, Aliotta, M, Ananna, C, Barbieri, L, Barile, F, Bemmerer, D, Best, A, Broggini, C, Bruno, CG, Caciolli, A, Campostrini, M, Casaburo, F, Cavanna, F, Colombetti, P, Compagnucci, A, Corvisiero, P, Csedreki, L, Davinson, T, De Gregorio, GM, Dell' Aquila, D, Depalo, R, Di Leva, A, Elekes, Z, Ferraro, F, Formicola, A, Fulop, Z, Gervino, G, Guglielmetti, A, Gustavino, C, Gyurky, G, Imbriani, G, Junker, M, Lugaro, M, Marigo, P, Marsh, J, Masha, E, Menegazzo, R, Mercogliano, D, Paticchio, V, Perrino, R, Prati, P, Rigato, V, Robb, D, Schiavulli, L, Sidhu, RS, Skowronski, J, Straniero, O, Szucs, T & Zavatarelli, S 2024, 'First direct measurement of the 64.5 keV resonance strength in the 17O(𝑝,𝛾)18F reaction', Physical Review Letters, vol. 133, no. 5, 052701, pp. 1-6. https://doi.org/10.1103/PhysRevLett.133.052701

TY - JOUR

T1 - First direct measurement of the 64.5 keV resonance strength in the 17O(𝑝,𝛾)18F reaction

AU - LUNA Collaboration

AU - Gesue, R M

AU - Ciani, G F

AU - Piatti, D

AU - Boeltzig, A

AU - Rapagnani, D.

AU - Aliotta, M.

AU - Ananna, C.

AU - Barbieri, L.

AU - Barile, F

AU - Bemmerer, D

AU - Best, A

AU - Broggini, C

AU - Bruno, C. G.

AU - Caciolli, A

AU - Campostrini, M.

AU - Casaburo, F.

AU - Cavanna, F

AU - Colombetti, P

AU - Compagnucci, A.

AU - Corvisiero, P

AU - Csedreki, L.

AU - Davinson, T.

AU - De Gregorio, G.M.

AU - Dell' Aquila, D.

AU - Depalo, R

AU - Di Leva, A

AU - Elekes, Z

AU - Ferraro, F

AU - Formicola, A

AU - Fulop, Zs

AU - Gervino, G

AU - Guglielmetti, A

AU - Gustavino, C

AU - Gyurky, Gy

AU - Imbriani, G

AU - Junker, M

AU - Lugaro, M

AU - Marigo, P

AU - Marsh, J.

AU - Masha, E

AU - Menegazzo, R

AU - Mercogliano, D

AU - Paticchio, V

AU - Perrino, R

AU - Prati, P

AU - Rigato, V.

AU - Robb, D.

AU - Schiavulli, L

AU - Sidhu, R.S.

AU - Skowronski, J.

AU - Straniero, O

AU - Szucs, T

AU - Zavatarelli, S

PY - 2024/8/2

Y1 - 2024/8/2

N2 - The CNO cycle is one of the most important nuclear energy sources in stars. At temperaturesof hydrostatic H-burning (20 MK < T < 80 MK) the 17O(p,γ) 18F reaction rate is dominated bythe poorly constrained 64.5 keV resonance. Here we report on the first direct measurements of its resonance strength and of the direct capture contribution at 142 keV, performed with a new high sensitivity setup at LUNA. The present resonance strength of ωγ(p,γ) bare = (30 ± 6stat ± 2syst) peV is about a factor of 2 higher than the values in literature, leading to a Γp bare = (34 ± 7stat ±3syst) neV, in agreement with LUNA result from the (p,α) channel. Such agreement strengthenour understanding of the oxygen isotopic ratios measured in red giant stars and in O-rich presolar grains.

AB - The CNO cycle is one of the most important nuclear energy sources in stars. At temperaturesof hydrostatic H-burning (20 MK < T < 80 MK) the 17O(p,γ) 18F reaction rate is dominated bythe poorly constrained 64.5 keV resonance. Here we report on the first direct measurements of its resonance strength and of the direct capture contribution at 142 keV, performed with a new high sensitivity setup at LUNA. The present resonance strength of ωγ(p,γ) bare = (30 ± 6stat ± 2syst) peV is about a factor of 2 higher than the values in literature, leading to a Γp bare = (34 ± 7stat ±3syst) neV, in agreement with LUNA result from the (p,α) channel. Such agreement strengthenour understanding of the oxygen isotopic ratios measured in red giant stars and in O-rich presolar grains.

U2 - 10.1103/PhysRevLett.133.052701

DO - 10.1103/PhysRevLett.133.052701

M3 - Article

SN - 0031-9007

VL - 133

SP - 1

EP - 6

JO - Physical Review Letters

JF - Physical Review Letters

IS - 5

M1 - 052701

ER -

First direct measurement of the 64.5 keV resonance strength in the 17O(𝑝,𝛾)18F reaction

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Edinburgh Nuclear Physics Group Consolidated Grant Proposal

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