Abstract
The20Ne(p,γ)21Na is the first reaction of the NeNa cycle and having the slowest reaction rate, it controls the speed at which the entire cycle proceeds. This reaction is important in different stellar scenarios such as red giants stars (during H shell-burning), asymptotic giant branch stars, novae, and massive stars. Existing uncertainties on the20Ne(p,γ)21Na are now the ones that severely affect the estimated elements production in the NeNa cycle. In particular, such uncertainties affect the amount of produced22Na, a stellarγ-ray signature, and22Ne, an important neutron source in the s-process, via the22Ne(α,n)25Mg. Here, we propose to study the resonance atER= 366 keV and to measure the20Ne(p,γ)21Na reaction cross section at proton energies below 400 keV, in particular the contribution from the sub-threshold state, in order to better constrain the overall astrophysical rate of this important reaction. In this contribution, the experimental setup will be described and the expected results discussed.
Highlights
The NeNa-MgAl cycles are involved in the synthesis of Ne, Na, and Mg isotopes
The 20Ne(p,γ)21Na is the first reaction of the NeNa cycle and having the slowest reaction rate, it controls the speed at which the entire cycle proceeds
This reaction is important in different stellar scenarios such as red giants stars, asymptotic giant branch stars, novae, and massive stars
Summary
The NeNa-MgAl cycles are involved in the synthesis of Ne, Na, and Mg isotopes. Proton capture on 20Ne nuclei may occur in different stellar scenarios such as red giants stars (during H shell-burning), asymptotic giant branch stars, novae, and massive stars. This reaction is important in different stellar scenarios such as red giants stars (during H shell-burning), asymptotic giant branch stars, novae, and massive stars. Existing uncertainties on the 20Ne(p,γ)21Na are the ones that severely affect the estimated elements production in the NeNa cycle.
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