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Cross section of the reaction 18O(p,γ)19F at astrophysical energies: The 90 keV resonance and the direct capture component

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  • A. Best
  • F R Pantaleo
  • A. Boeltzig
  • Gianluca Imbriani
  • J Balibrea-Correa
  • D. Bemmerer
  • C. Broggini
  • R. Buompane
  • A Caciolli
  • F. Cavanna
  • Thomas Chillery
  • G. F. Ciani
  • P Corvisiero
  • L. Csedreki
  • R. J. deBoer
  • R Depalo
  • A Di Leva
  • Z Elekes
  • F Ferraro
  • E. M. Fiore
  • A Formicola
  • Zs Fülöp
  • G Gervino
  • A Guglielmetti
  • C Gustavino
  • Gy Gyürky
  • M. Junker
  • I. Kochanek
  • M. Lugaro
  • P. Marigo
  • R Menegazzo
  • V Mossa
  • V Paticchio
  • R Perrino
  • D. Piatti
  • P Prati
  • L. Schiavulli
  • K. Stöckel
  • O Straniero
  • F Strieder
  • T Szücs
  • M. P. Takács
  • Davide Trezzi
  • M Wiescher
  • S Zavatarelli

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https://www.sciencedirect.com/science/article/pii/S0370269319306227
Original languageEnglish
Article number134900
JournalPhysics Letters B
Volume797
Early online date30 Aug 2019
DOIs
Publication statusPublished - 10 Oct 2019

Abstract

The observation of oxygen isotopes in giant stars sheds light on mixing processes operating in their interiors. Due to the very strong correlation between nuclear burning and mixing processes it is very important to reduce the uncertainty on the cross sections of the nuclear reactions that are involved. In this paper we focus our attention on the reaction 18O(p,)19F. While the 18O(p, )15N channel is thought to be dominant, the (p,) channel can still be an important
component in stellar burning in giants, depending on the low energy cross section. So far only extrapolations from higher-energy measurements exist and recent estimates vary by orders of magnitude. These large uncertainties call for an experimental reinvestigation of this reaction. We present a direct measurement of the 18O(p;)19F cross section using a high-eciency 4 BGO summing detector at the Laboratory for Underground Nuclear Astrophysics (LUNA). The reaction cross section has been directly determined for the rst time from 140 keV down to 85 keV and the dierent cross section components have been obtained individually. The previously highly uncertain strength of the 90 keV resonance was found to be 0.53 0.07 neV, three orders of magnitude lower than an indirect estimate based on nuclear properties of the resonant state and a factor of 20 lower than a recently established upper limit, excluding the possibility that the 90 keV resonance can contribute signicantly to the stellar reaction rate.

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