Direct Measurement of the ^{13}C(α,n)^{16}O Cross Section into the s-Process Gamow Peak.

  title={Direct Measurement of the ^\{13\}C($\alpha$,n)^\{16\}O Cross Section into the s-Process Gamow Peak.},
  author={Giovanni Francesco Ciani and Laszlo Csedreki and D. Rapagnani and M Aliotta and J. Balibrea-Correa and Francesco Barile and Daniel Bemmerer and A. Best and Axel Boeltzig and Carlo Broggini and Carlo Giulio Bruno and Antonio Caciolli and Francesca Cavanna and T Chillery and Paolo Colombetti and Pietro Corvisiero and Sergio Cristallo and T. Davinson and Rosanna Depalo and A. Di Leva and Zolt{\'a}n Elekes and F Ferraro and Enrichetta Maria Fiore and Alba Formicola and Zs. F{\"u}l{\"o}p and G. P. Gervino and Alessandra Guglielmetti and C Gustavino and Gy. Gy{\"u}rky and Gianluca Imbriani and M Junker and Maria Lugaro and P. Marigo and Eliana Masha and R. Menegazzo and Viviana Mossa and Felice Pantaleo and Vincenzo Paticchio and Roberto Perrino and Denise Piatti and Paolo Prati and Luigi Schiavulli and Klaus St{\"o}ckel and Oscar Straniero and T. Sz{\"u}cs and M. P. Tak{\'a}cs and F. Terrasi and Diego Vescovi and S Zavatarelli},
  journal={Physical review letters},
  volume={127 15},
One of the main neutron sources for the astrophysical s process is the reaction ^{13}C(α,n)^{16}O, taking place in thermally pulsing asymptotic giant branch stars at temperatures around 90 MK. To model the nucleosynthesis during this process the reaction cross section needs to be known in the 150-230 keV energy window (Gamow peak). At these sub-Coulomb energies, cross section direct measurements are severely affected by the low event rate, making us rely on input from indirect methods and… 

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