Underground study of the O-17(p,gamma) F-18 reaction relevant for explosive hydrogen burning

Luna Collaboration; A. Di Leva; D. A. Scott; A. Caciolli; A. Formicola; F. Strieder; M. Aliotta; M. Anders; D. Bemmerer; C. Broggini; P. Corvisiero; Z. Elekes; Zs. Fueloep; G. Gervino; A. Guglielmetti; C. Gustavino; Gy. Gyuerky; G. Imbriani; J. Jose; M. Junker; M. Laubenstein; R. Menegazzo; E. Napolitani; P. Prati; V. Rigato; V. Roca; E. Somorjai; C. Salvo; O. Straniero; T. Szuecs; F. Terrasi; D. Trezzi

doi:10.1103/PhysRevC.89.015803

Underground study of the O-17(p,gamma) F-18 reaction relevant for explosive hydrogen burning

Luna Collaboration, A. Di Leva^*, D. A. Scott, A. Caciolli, A. Formicola, F. Strieder, M. Aliotta, M. Anders, D. Bemmerer, C. Broggini, P. Corvisiero, Z. Elekes, Zs. Fueloep, G. Gervino, A. Guglielmetti, C. Gustavino, Gy. Gyuerky, G. Imbriani, J. Jose, M. JunkerM. Laubenstein, R. Menegazzo, E. Napolitani, P. Prati, V. Rigato, V. Roca, E. Somorjai, C. Salvo, O. Straniero, T. Szuecs, F. Terrasi, D. Trezzi

^*Corresponding author for this work

School of Physics and Astronomy

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

Abstract / Description of output

Background: The O-17( p,gamma)F-18 reaction affects the production of key isotopes ( e.g., F-18 and O-18) in the explosive hydrogen burning that powers classical novae. Under these explosive conditions, the reaction rate is dominated by contributions from a narrow resonance at E-c.m. = 183 keV and by the combined contributions of direct capture and low-energy tails of broad resonances. At present, the astrophysical reaction rate is not well constrained because of the lack of data in the energy region appropriate to classical novae.

Purpose: This study aims at the measurement of the O-17( p,gamma)F-18 reaction cross section in order to determine its reaction rate in the temperature region appropriate to explosive hydrogen burning in novae.

Method: The O-17( p,gamma)F-18 reaction cross section was measured using both the prompt detection of the emitted gamma rays and an activation technique. Measurements were carried out at the Laboratory for Underground Nuclear Astrophysics ( Gran Sasso, Italy) where the strongly reduced cosmic-ray-induced background allows for improved sensitivity compared to previous studies.

Results: The O-17( p,gamma)F-18 reaction cross section was measured in the range E-c.m. = 160 to 370 keV. The strength of the E-c.m. = 183 keV resonance, omega gamma = 1.67 +/- 0.12 mu eV, was determined with unprecedented precision. The total S factor was obtained through a combined fit of prompt gamma-ray and activation results. An overall global fit including other existing data sets was also carried out and a recommended astrophysical reaction rate is presented.

Conclusions: The reaction rate uncertainty attained in this work is now below the required precision for nova models. We verified, following a full set of hydrodynamic nova models, that the abundances of oxygen and fluorine isotopes obtained with the present reaction rate are determined with 10% precision and put firmer constraints on observational signatures of novae events.

Original language	English
Article number	015803
Number of pages	15
Journal	Physical Review C
Volume	89
Issue number	1
DOIs	https://doi.org/10.1103/PhysRevC.89.015803
Publication status	Published - 21 Jan 2014

Keywords / Materials (for Non-textual outputs)

INTERMEDIATE-MASS STARS
CLASSICAL NOVAE
NUCLEAR ASTROPHYSICS
PRESOLAR GRAINS
REACTION-RATES
WHITE-DWARFS
S-FACTOR
NUCLEOSYNTHESIS
EVOLUTION
MODELS

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10.1103/PhysRevC.89.015803

Marialuisa Aliotta
- m.aliottaed.acuk
- School of Physics and Astronomy - Personal Chair in Experimental Nuclear Astrophysics
Person: Academic: Research Active

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Luna Collaboration, Di Leva, A., Scott, D. A., Caciolli, A., Formicola, A., Strieder, F., Aliotta, M., Anders, M., Bemmerer, D., Broggini, C., Corvisiero, P., Elekes, Z., Fueloep, Z., Gervino, G., Guglielmetti, A., Gustavino, C., Gyuerky, G., Imbriani, G., Jose, J., ... Trezzi, D. (2014). Underground study of the O-17(p,gamma) F-18 reaction relevant for explosive hydrogen burning. Physical Review C, 89(1), Article 015803. https://doi.org/10.1103/PhysRevC.89.015803

@article{69347573d5494b8aab6b8f9d8e0d3bfa,

title = "Underground study of the O-17(p,gamma) F-18 reaction relevant for explosive hydrogen burning",

abstract = "Background: The O-17( p,gamma)F-18 reaction affects the production of key isotopes ( e.g., F-18 and O-18) in the explosive hydrogen burning that powers classical novae. Under these explosive conditions, the reaction rate is dominated by contributions from a narrow resonance at E-c.m. = 183 keV and by the combined contributions of direct capture and low-energy tails of broad resonances. At present, the astrophysical reaction rate is not well constrained because of the lack of data in the energy region appropriate to classical novae.Purpose: This study aims at the measurement of the O-17( p,gamma)F-18 reaction cross section in order to determine its reaction rate in the temperature region appropriate to explosive hydrogen burning in novae.Method: The O-17( p,gamma)F-18 reaction cross section was measured using both the prompt detection of the emitted gamma rays and an activation technique. Measurements were carried out at the Laboratory for Underground Nuclear Astrophysics ( Gran Sasso, Italy) where the strongly reduced cosmic-ray-induced background allows for improved sensitivity compared to previous studies.Results: The O-17( p,gamma)F-18 reaction cross section was measured in the range E-c.m. = 160 to 370 keV. The strength of the E-c.m. = 183 keV resonance, omega gamma = 1.67 +/- 0.12 mu eV, was determined with unprecedented precision. The total S factor was obtained through a combined fit of prompt gamma-ray and activation results. An overall global fit including other existing data sets was also carried out and a recommended astrophysical reaction rate is presented.Conclusions: The reaction rate uncertainty attained in this work is now below the required precision for nova models. We verified, following a full set of hydrodynamic nova models, that the abundances of oxygen and fluorine isotopes obtained with the present reaction rate are determined with 10% precision and put firmer constraints on observational signatures of novae events.",

keywords = "INTERMEDIATE-MASS STARS, CLASSICAL NOVAE, NUCLEAR ASTROPHYSICS, PRESOLAR GRAINS, REACTION-RATES, WHITE-DWARFS, S-FACTOR, NUCLEOSYNTHESIS, EVOLUTION, MODELS",

author = "{Luna Collaboration} and {Di Leva}, A. and Scott, {D. A.} and A. Caciolli and A. Formicola and F. Strieder and M. Aliotta and M. Anders and D. Bemmerer and C. Broggini and P. Corvisiero and Z. Elekes and Zs. Fueloep and G. Gervino and A. Guglielmetti and C. Gustavino and Gy. Gyuerky and G. Imbriani and J. Jose and M. Junker and M. Laubenstein and R. Menegazzo and E. Napolitani and P. Prati and V. Rigato and V. Roca and E. Somorjai and C. Salvo and O. Straniero and T. Szuecs and F. Terrasi and D. Trezzi",

year = "2014",

month = jan,

day = "21",

doi = "10.1103/PhysRevC.89.015803",

language = "English",

volume = "89",

journal = "Physical Review C",

issn = "0556-2813",

publisher = "American Physical Society",

number = "1",

}

Luna Collaboration, Di Leva, A, Scott, DA, Caciolli, A, Formicola, A, Strieder, F, Aliotta, M, Anders, M, Bemmerer, D, Broggini, C, Corvisiero, P, Elekes, Z, Fueloep, Z, Gervino, G, Guglielmetti, A, Gustavino, C, Gyuerky, G, Imbriani, G, Jose, J, Junker, M, Laubenstein, M, Menegazzo, R, Napolitani, E, Prati, P, Rigato, V, Roca, V, Somorjai, E, Salvo, C, Straniero, O, Szuecs, T, Terrasi, F & Trezzi, D 2014, 'Underground study of the O-17(p,gamma) F-18 reaction relevant for explosive hydrogen burning', Physical Review C, vol. 89, no. 1, 015803. https://doi.org/10.1103/PhysRevC.89.015803

TY - JOUR

T1 - Underground study of the O-17(p,gamma) F-18 reaction relevant for explosive hydrogen burning

AU - Luna Collaboration

AU - Di Leva, A.

AU - Scott, D. A.

AU - Caciolli, A.

AU - Formicola, A.

AU - Strieder, F.

AU - Aliotta, M.

AU - Anders, M.

AU - Bemmerer, D.

AU - Broggini, C.

AU - Corvisiero, P.

AU - Elekes, Z.

AU - Fueloep, Zs.

AU - Gervino, G.

AU - Guglielmetti, A.

AU - Gustavino, C.

AU - Gyuerky, Gy.

AU - Imbriani, G.

AU - Jose, J.

AU - Junker, M.

AU - Laubenstein, M.

AU - Menegazzo, R.

AU - Napolitani, E.

AU - Prati, P.

AU - Rigato, V.

AU - Roca, V.

AU - Somorjai, E.

AU - Salvo, C.

AU - Straniero, O.

AU - Szuecs, T.

AU - Terrasi, F.

AU - Trezzi, D.

PY - 2014/1/21

Y1 - 2014/1/21

N2 - Background: The O-17( p,gamma)F-18 reaction affects the production of key isotopes ( e.g., F-18 and O-18) in the explosive hydrogen burning that powers classical novae. Under these explosive conditions, the reaction rate is dominated by contributions from a narrow resonance at E-c.m. = 183 keV and by the combined contributions of direct capture and low-energy tails of broad resonances. At present, the astrophysical reaction rate is not well constrained because of the lack of data in the energy region appropriate to classical novae.Purpose: This study aims at the measurement of the O-17( p,gamma)F-18 reaction cross section in order to determine its reaction rate in the temperature region appropriate to explosive hydrogen burning in novae.Method: The O-17( p,gamma)F-18 reaction cross section was measured using both the prompt detection of the emitted gamma rays and an activation technique. Measurements were carried out at the Laboratory for Underground Nuclear Astrophysics ( Gran Sasso, Italy) where the strongly reduced cosmic-ray-induced background allows for improved sensitivity compared to previous studies.Results: The O-17( p,gamma)F-18 reaction cross section was measured in the range E-c.m. = 160 to 370 keV. The strength of the E-c.m. = 183 keV resonance, omega gamma = 1.67 +/- 0.12 mu eV, was determined with unprecedented precision. The total S factor was obtained through a combined fit of prompt gamma-ray and activation results. An overall global fit including other existing data sets was also carried out and a recommended astrophysical reaction rate is presented.Conclusions: The reaction rate uncertainty attained in this work is now below the required precision for nova models. We verified, following a full set of hydrodynamic nova models, that the abundances of oxygen and fluorine isotopes obtained with the present reaction rate are determined with 10% precision and put firmer constraints on observational signatures of novae events.

AB - Background: The O-17( p,gamma)F-18 reaction affects the production of key isotopes ( e.g., F-18 and O-18) in the explosive hydrogen burning that powers classical novae. Under these explosive conditions, the reaction rate is dominated by contributions from a narrow resonance at E-c.m. = 183 keV and by the combined contributions of direct capture and low-energy tails of broad resonances. At present, the astrophysical reaction rate is not well constrained because of the lack of data in the energy region appropriate to classical novae.Purpose: This study aims at the measurement of the O-17( p,gamma)F-18 reaction cross section in order to determine its reaction rate in the temperature region appropriate to explosive hydrogen burning in novae.Method: The O-17( p,gamma)F-18 reaction cross section was measured using both the prompt detection of the emitted gamma rays and an activation technique. Measurements were carried out at the Laboratory for Underground Nuclear Astrophysics ( Gran Sasso, Italy) where the strongly reduced cosmic-ray-induced background allows for improved sensitivity compared to previous studies.Results: The O-17( p,gamma)F-18 reaction cross section was measured in the range E-c.m. = 160 to 370 keV. The strength of the E-c.m. = 183 keV resonance, omega gamma = 1.67 +/- 0.12 mu eV, was determined with unprecedented precision. The total S factor was obtained through a combined fit of prompt gamma-ray and activation results. An overall global fit including other existing data sets was also carried out and a recommended astrophysical reaction rate is presented.Conclusions: The reaction rate uncertainty attained in this work is now below the required precision for nova models. We verified, following a full set of hydrodynamic nova models, that the abundances of oxygen and fluorine isotopes obtained with the present reaction rate are determined with 10% precision and put firmer constraints on observational signatures of novae events.

KW - INTERMEDIATE-MASS STARS

KW - CLASSICAL NOVAE

KW - NUCLEAR ASTROPHYSICS

KW - PRESOLAR GRAINS

KW - REACTION-RATES

KW - WHITE-DWARFS

KW - S-FACTOR

KW - NUCLEOSYNTHESIS

KW - EVOLUTION

KW - MODELS

U2 - 10.1103/PhysRevC.89.015803

DO - 10.1103/PhysRevC.89.015803

M3 - Article

SN - 0556-2813

VL - 89

JO - Physical Review C

JF - Physical Review C

IS - 1

M1 - 015803

ER -

Underground study of the O-17(p,gamma) F-18 reaction relevant for explosive hydrogen burning

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