First measurement of the 14N(p,γ)15O cross section down to 70 keV

A. Lemut, D. Bemmerer, F. Confortola, R. Bonetti, C. Broggini, P. Corvisiero, H. Costantini, J. Cruz, A. Formicola, Zs. S. Fülöp, G. Gervino, A. Guglielmetti, C. Gustavino, G. Gyürky, G. Imbriani, A. P. Jesus, M. Junker, B. Limata, R. Menegazzo, P. PratiV. Roca, D. Rogalla, C. Rolfs, M. Romano, C. Rossi Alvarez, F. Schümann, E. Somorjai, O. Straniero, F. Strieder, F. Terrasi, H. P. Trautvetter

Research output: Contribution to journalArticle

122 Citations (Scopus)

Abstract

In stars with temperatures above 20×106 K, hydrogen burning is dominated by the CNO cycle. Its rate is determined by the slowest process, the 14N(p, γ)15O reaction. Deep underground in Italy's Gran Sasso laboratory, at the LUNA 400 kV accelerator, the cross section of this reaction has been measured at energies much lower than ever achieved before. Using a windowless gas target and a 4π BGO summing detector, direct cross section data has been obtained down to 70 keV, reaching a value of 0.24 picobarn. The Gamow peak has been covered by experimental data for several scenarios of stable and explosive hydrogen burning. In addition, the strength of the 259 keV resonance has been remeasured. The thermonuclear reaction rate has been calculated for temperatures 90-300×106 K, for the first time with negligible impact from extrapolations.

Original languageEnglish
Pages (from-to)483-487
Number of pages5
JournalPhysics Letters B
Volume634
Issue number5-6
DOIs
Publication statusPublished - Mar 23 2006

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thermonuclear reactions
cross sections
hydrogen
Italy
extrapolation
reaction kinetics
accelerators
stars
cycles
temperature
detectors
gases
energy

Keywords

  • N(p, γ)O
  • AGB stars
  • CNO cycle
  • Cross section measurement
  • Hydrogen shell burning
  • Radiative capture
  • Underground nuclear astrophysics

ASJC Scopus subject areas

  • Nuclear and High Energy Physics

Cite this

Lemut, A., Bemmerer, D., Confortola, F., Bonetti, R., Broggini, C., Corvisiero, P., ... Trautvetter, H. P. (2006). First measurement of the 14N(p,γ)15O cross section down to 70 keV. Physics Letters B, 634(5-6), 483-487. https://doi.org/10.1016/j.physletb.2006.02.021

First measurement of the 14N(p,γ)15O cross section down to 70 keV. / Lemut, A.; Bemmerer, D.; Confortola, F.; Bonetti, R.; Broggini, C.; Corvisiero, P.; Costantini, H.; Cruz, J.; Formicola, A.; Fülöp, Zs. S.; Gervino, G.; Guglielmetti, A.; Gustavino, C.; Gyürky, G.; Imbriani, G.; Jesus, A. P.; Junker, M.; Limata, B.; Menegazzo, R.; Prati, P.; Roca, V.; Rogalla, D.; Rolfs, C.; Romano, M.; Rossi Alvarez, C.; Schümann, F.; Somorjai, E.; Straniero, O.; Strieder, F.; Terrasi, F.; Trautvetter, H. P.

In: Physics Letters B, Vol. 634, No. 5-6, 23.03.2006, p. 483-487.

Research output: Contribution to journalArticle

Lemut, A, Bemmerer, D, Confortola, F, Bonetti, R, Broggini, C, Corvisiero, P, Costantini, H, Cruz, J, Formicola, A, Fülöp, ZS, Gervino, G, Guglielmetti, A, Gustavino, C, Gyürky, G, Imbriani, G, Jesus, AP, Junker, M, Limata, B, Menegazzo, R, Prati, P, Roca, V, Rogalla, D, Rolfs, C, Romano, M, Rossi Alvarez, C, Schümann, F, Somorjai, E, Straniero, O, Strieder, F, Terrasi, F & Trautvetter, HP 2006, 'First measurement of the 14N(p,γ)15O cross section down to 70 keV', Physics Letters B, vol. 634, no. 5-6, pp. 483-487. https://doi.org/10.1016/j.physletb.2006.02.021
Lemut A, Bemmerer D, Confortola F, Bonetti R, Broggini C, Corvisiero P et al. First measurement of the 14N(p,γ)15O cross section down to 70 keV. Physics Letters B. 2006 Mar 23;634(5-6):483-487. https://doi.org/10.1016/j.physletb.2006.02.021
Lemut, A. ; Bemmerer, D. ; Confortola, F. ; Bonetti, R. ; Broggini, C. ; Corvisiero, P. ; Costantini, H. ; Cruz, J. ; Formicola, A. ; Fülöp, Zs. S. ; Gervino, G. ; Guglielmetti, A. ; Gustavino, C. ; Gyürky, G. ; Imbriani, G. ; Jesus, A. P. ; Junker, M. ; Limata, B. ; Menegazzo, R. ; Prati, P. ; Roca, V. ; Rogalla, D. ; Rolfs, C. ; Romano, M. ; Rossi Alvarez, C. ; Schümann, F. ; Somorjai, E. ; Straniero, O. ; Strieder, F. ; Terrasi, F. ; Trautvetter, H. P. / First measurement of the 14N(p,γ)15O cross section down to 70 keV. In: Physics Letters B. 2006 ; Vol. 634, No. 5-6. pp. 483-487.
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abstract = "In stars with temperatures above 20×106 K, hydrogen burning is dominated by the CNO cycle. Its rate is determined by the slowest process, the 14N(p, γ)15O reaction. Deep underground in Italy's Gran Sasso laboratory, at the LUNA 400 kV accelerator, the cross section of this reaction has been measured at energies much lower than ever achieved before. Using a windowless gas target and a 4π BGO summing detector, direct cross section data has been obtained down to 70 keV, reaching a value of 0.24 picobarn. The Gamow peak has been covered by experimental data for several scenarios of stable and explosive hydrogen burning. In addition, the strength of the 259 keV resonance has been remeasured. The thermonuclear reaction rate has been calculated for temperatures 90-300×106 K, for the first time with negligible impact from extrapolations.",
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AU - Lemut, A.

AU - Bemmerer, D.

AU - Confortola, F.

AU - Bonetti, R.

AU - Broggini, C.

AU - Corvisiero, P.

AU - Costantini, H.

AU - Cruz, J.

AU - Formicola, A.

AU - Fülöp, Zs. S.

AU - Gervino, G.

AU - Guglielmetti, A.

AU - Gustavino, C.

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AU - Imbriani, G.

AU - Jesus, A. P.

AU - Junker, M.

AU - Limata, B.

AU - Menegazzo, R.

AU - Prati, P.

AU - Roca, V.

AU - Rogalla, D.

AU - Rolfs, C.

AU - Romano, M.

AU - Rossi Alvarez, C.

AU - Schümann, F.

AU - Somorjai, E.

AU - Straniero, O.

AU - Strieder, F.

AU - Terrasi, F.

AU - Trautvetter, H. P.

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N2 - In stars with temperatures above 20×106 K, hydrogen burning is dominated by the CNO cycle. Its rate is determined by the slowest process, the 14N(p, γ)15O reaction. Deep underground in Italy's Gran Sasso laboratory, at the LUNA 400 kV accelerator, the cross section of this reaction has been measured at energies much lower than ever achieved before. Using a windowless gas target and a 4π BGO summing detector, direct cross section data has been obtained down to 70 keV, reaching a value of 0.24 picobarn. The Gamow peak has been covered by experimental data for several scenarios of stable and explosive hydrogen burning. In addition, the strength of the 259 keV resonance has been remeasured. The thermonuclear reaction rate has been calculated for temperatures 90-300×106 K, for the first time with negligible impact from extrapolations.

AB - In stars with temperatures above 20×106 K, hydrogen burning is dominated by the CNO cycle. Its rate is determined by the slowest process, the 14N(p, γ)15O reaction. Deep underground in Italy's Gran Sasso laboratory, at the LUNA 400 kV accelerator, the cross section of this reaction has been measured at energies much lower than ever achieved before. Using a windowless gas target and a 4π BGO summing detector, direct cross section data has been obtained down to 70 keV, reaching a value of 0.24 picobarn. The Gamow peak has been covered by experimental data for several scenarios of stable and explosive hydrogen burning. In addition, the strength of the 259 keV resonance has been remeasured. The thermonuclear reaction rate has been calculated for temperatures 90-300×106 K, for the first time with negligible impact from extrapolations.

KW - N(p, γ)O

KW - AGB stars

KW - CNO cycle

KW - Cross section measurement

KW - Hydrogen shell burning

KW - Radiative capture

KW - Underground nuclear astrophysics

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