O Hydrogen Burning at the Energies of Classical Nova at Luna

@inproceedings{Caciolli2015OHB,
  title={O Hydrogen Burning at the Energies of Classical Nova at Luna},
  author={A. Caciolli and D. A. Scott and Agnese Di Leva and Carlo Bruno},
  year={2015}
}
cluding red giants, asymptotic giant branch (AGB) stars, massive stars, and classical novae. In particular, the ratio between reaction rates of 17O(p,α)14N (Q = 1.2 MeV) and 17O(p,γ)18F (Q = 5.6 MeV) channels on 17O is one of the most important parameters for the galactic synthesis of 17O, the stellar production of radioactive 18F, and for predicted O isotopic ratios in presolar grains. The LUNA collaboration has studied the 17O(p,γ)18F in a wide energy range (from 167