The 22Ne(p,γ)23Na is a reaction of the NeNa cycle of stellar hydrogen burning. This cycle is active in the Red Giant Branch and Asymptotic Giant Branch stars, as well as in novae explosions. In particular, it rules the abundance of the elements between 20Ne and 27Al. Furthermore, the proton capture on 22Ne may have an impact on the production of 23Na in type Ia supernovae, with a possible link to the 56Ni yield. The amount of 56Ni determines the light curve of these supernovae, used as standard candles in cosmology. The 22Ne(p,γ)23Na reaction rate is highly uncertain because of a large number of yet unobserved resonances in the energy region of the Gamow peak. A study of the 22Ne(p,γ)23Na is on-going at LUNA in Gran Sasso. The results of a feasibility test, as well as the measurement strategy and the setup for the first experimental campaign are discussed.

Towards a study of 22Ne(p,γ)23Na at LUNA in Gran Sasso / R. Depalo. - In: POS PROCEEDINGS OF SCIENCE. - ISSN 1824-8039. - 196:(2014), pp. 068.1-068.4. ((Intervento presentato al 15. convegno International Workshop on Neutrino Telescopes tenutosi a Trieste nel 2013.

Towards a study of 22Ne(p,γ)23Na at LUNA in Gran Sasso

R. Depalo
2014

Abstract

The 22Ne(p,γ)23Na is a reaction of the NeNa cycle of stellar hydrogen burning. This cycle is active in the Red Giant Branch and Asymptotic Giant Branch stars, as well as in novae explosions. In particular, it rules the abundance of the elements between 20Ne and 27Al. Furthermore, the proton capture on 22Ne may have an impact on the production of 23Na in type Ia supernovae, with a possible link to the 56Ni yield. The amount of 56Ni determines the light curve of these supernovae, used as standard candles in cosmology. The 22Ne(p,γ)23Na reaction rate is highly uncertain because of a large number of yet unobserved resonances in the energy region of the Gamow peak. A study of the 22Ne(p,γ)23Na is on-going at LUNA in Gran Sasso. The results of a feasibility test, as well as the measurement strategy and the setup for the first experimental campaign are discussed.
Settore FIS/04 - Fisica Nucleare e Subnucleare
https://pos.sissa.it/196/068/
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/2434/931204
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