Abstract
The 22 Ne(p, ) 23 Na reaction is involved in the hydrogen burning neon-sodium cycle. In second-generation stars, where the central temperature is higher than 0.05 10 9 K, hydrogen burning can proceed also via the NeNa cycle. The 22 Ne(p, ) 23 Na cross section, dominated by a large number of resonances never measured directly, is still a ected by large uncertainties. At the Laboratory for Underground Nuclear Astrophysics (LUNA), in the Gran Sasso National Laboratory in Italy, several cross sections have been measured in the past down to the energies of astrophysical interest. An experimental study of the 22 Ne(p, ) 23 Na reaction is under preparation at LUNA, using a windowless gas target system and two HPGe detectors.
Highlights
The NeNa cycle determines the nucleosynthesis of the Ne and Na isotopes in the Red Giant Branch and Asymptotic Giant Branch phases of stellar evolution [1]
The NeNa cycle affects the abundances of the elements between 20Ne and 27Al ejected in the interstellar medium by classical novae explosions [2]
The following reactions are involved in this cycle [3]: 20Ne(p,γ)21Na(β+,ν)21Ne(p,γ)22Na(β+,ν)22Ne(p,γ)23Na(p,α)20Ne From the astrophysical point of view, the 22Ne(p,γ)23Na cross section measurement is important for studying:
Summary
The NeNa cycle determines the nucleosynthesis of the Ne and Na isotopes in the Red Giant Branch and Asymptotic Giant Branch phases of stellar evolution [1]. The following reactions are involved in this cycle [3]: 20Ne(p,γ)21Na(β+,ν)21Ne(p,γ)22Na(β+,ν)22Ne(p,γ)23Na(p,α)20Ne From the astrophysical point of view, the 22Ne(p,γ)23Na cross section measurement is important for studying: the Red Giant Branch Stars surface composition (Gamow Peak 30 keV < E < 100 keV) the composition of ejected materials from Asymptotic Giant Branch Stars and Classical Novae (Gamow Peak 100 keV < E < 400 keV) The cross section of a charged particle induced reaction steeply drops with decreasing energy due to the Coulomb barrier It has a very low value at the Gamow Peak; this prevents a direct measurement in a laboratory on the Earth’s surface, where the signal to background ratio is too small because of cosmic ray interactions with detectors. Angular distribution measurements can be made by placing the detector at different angles with respect to the ion beam
Sign-in/Register to view highlights & summary Sign-in/Register to access full text options 
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a callDisclaimer: All third-party content on this website/platform is and will remain the property of their respective owners and is provided on "as is" basis without any warranties, express or implied. Use of third-party content does not indicate any affiliation, sponsorship with or endorsement by them. Any references to third-party content is to identify the corresponding services and shall be considered fair use under The CopyrightLaw.
