Category: p_g

2H(p,g)3He Mossa et al. 2020 Direct measurement performed at the Laboratory for Underground Nuclear Astrophysics (LUNA) of the Laboratori Nazionali del Gran Sasso (Italy). A high-purity deuterium gas target was bombarded with an intense proton beam from the LUNA 400-kilovolt accelerator and the γ-rays from the nuclear reaction were detected with a high-purity germanium detector.… Continue reading 2H(p,g)3He

15N(p,g)16O Caciolli et al. 2011 Direct measurement performed at LUNA covering for the first time the center of mass energy range 70−370 keV, which corresponds to stellar temperatures between 65 × 106 K and 780 × 106 K. This range includes the Gamow-peak energy of explosive H-burning taking place in the external layer of a nova… Continue reading 15N(p,g)16O

23Na(p,g)24Mg Boeltzig et al. 2019 Evaluation of the nuclear reaction rate based on measurements of the resonance strengths at Ep = 140 and 251keV, which are the main contributors to the reaction rate at 50 ≲ T ≲ 110MK, performed at the Laboratory for Underground Nuclear Astrophysics (LUNA). Two complementary detection approaches were used: high efficiency with… Continue reading 23Na(p,g)24Mg

20Ne(p,g)21Na Masha et al. 2023 Measurement of the nuclear reaction direct capture contribution, for the first time below Ec .m .=352 keV, and of the contribution from the Ec .m .=368 keV resonance, which dominates the reaction rate at T =0.03 -1.00 GK. The experiment was performed deep underground at the Laboratory for Underground Nuclear Astrophysics,… Continue reading 20Ne(p,g)21Na

18O(p,g)18F Best et al. 2019 Direct cross section measurement using a high-efficiency 4π BGO summing detector at the Laboratory for Underground Nuclear Astrophysics (LUNA). The reaction cross section was directly determined for the first time from 140 keV down to 85 keV and the different cross section components have been obtained individually. The previously highly uncertain strength of the… Continue reading 18O(p,g)18F

17O(p,g)18F Di Leva et al. 2014 The reaction cross section was measured using both the prompt detection of the emitted γ 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. Link… Continue reading 17O(p,g)18F

14N(p,g)15O Imbriani et al. 2005 Nuclear reaction rate based on the measurement of the astrophysical S(E) factor for effective center-of-mass energies between E eff = 119 and 367 keV at the LUNA facility. Link to the paper.  Nuclear reaction rate in the MESA format:

13C(p,g)14N Skowronski et al. 2023 Re-evaluated thermonuclear rate based on cross section measurements performed at the Laboratory for Underground Nuclear Astrophysics, down to the lowest energies to date (Ec.m.=60  keV)., hence reaching for the first time the high energy tail of hydrogen burning in the shell of giant stars. Compared with most of the previous literature, these… Continue reading 13C(p,g)14N

12C(p,g)13N Skowronski et al. 2023 Re-evaluated thermonuclear rate based on cross section measurements performed at the Laboratory for Underground Nuclear Astrophysics, down to the lowest energies to date (Ec.m.=60  keV)., hence reaching for the first time the high energy tail of hydrogen burning in the shell of giant stars. Compared with most of the previous literature, these… Continue reading 12C(p,g)13N

6Li(p,g)7Be Piatti et al. 2020 Re-evaluated thermonuclear rate based on cross section measurements performed at the Laboratory for Underground Nuclear Astrophysics, covering the center-of-mass energy range E=60-350 keV. Link to the paper. Nuclear reaction rate in the MESA format: