# Direct Measurement of the ^{13}C(α,n)^{16}O Cross Section into the s-Process Gamow Peak.

@article{Ciani2021DirectMO,
title={Direct Measurement of the ^\{13\}C($\alpha$,n)^\{16\}O Cross Section into the s-Process Gamow Peak.},
author={Giovanni Francesco Ciani and Laszlo Csedreki and D. Rapagnani and M Aliotta and J. Balibrea-Correa and Francesco Barile and Daniel Bemmerer and A. Best and Axel Boeltzig and Carlo Broggini and Carlo Giulio Bruno and Antonio Caciolli and Francesca Cavanna and T Chillery and Paolo Colombetti and Pietro Corvisiero and Sergio Cristallo and T. Davinson and Rosanna Depalo and A. Di Leva and Zolt{\'a}n Elekes and F Ferraro and Enrichetta Maria Fiore and Alba Formicola and Zs. F{\"u}l{\"o}p and G. P. Gervino and Alessandra Guglielmetti and C Gustavino and Gy. Gy{\"u}rky and Gianluca Imbriani and M Junker and Maria Lugaro and P. Marigo and Eliana Masha and R. Menegazzo and Viviana Mossa and Felice Pantaleo and Vincenzo Paticchio and Roberto Perrino and Denise Piatti and Paolo Prati and Luigi Schiavulli and Klaus St{\"o}ckel and Oscar Straniero and T. Sz{\"u}cs and M. P. Tak{\'a}cs and F. Terrasi and Diego Vescovi and S Zavatarelli},
journal={Physical review letters},
year={2021},
volume={127 15},
pages={
152701
}
}
One of the main neutron sources for the astrophysical s process is the reaction ^{13}C(α,n)^{16}O, taking place in thermally pulsing asymptotic giant branch stars at temperatures around 90 MK. To model the nucleosynthesis during this process the reaction cross section needs to be known in the 150-230 keV energy window (Gamow peak). At these sub-Coulomb energies, cross section direct measurements are severely affected by the low event rate, making us rely on input from indirect methods and…

## References

SHOWING 1-10 OF 24 REFERENCES
Concurrent Application of ANC and THM to assess the 13C(α, n)16O Absolute Cross Section at Astrophysical Energies and Possible Consequences for Neutron Production in Low-mass AGB Stars
• Physics
• 2017
The reaction is considered to be the main neutron source responsible for the production of heavy nuclides (from to ) through slow n-capture nucleosynthesis (s-process) at low temperatures during the
Reaction rates of the s-process neutron sources Ne-22(alpha, n)Mg-25 and C-13(alpha, n)O-16
The excitation function of the s-process neutron source reactions 22 Ne(α, n) 25 Mg and 13 C(α, n) 16 O has been measured using improved ion-beam, target, and detection techniques, reaching a
The branchings of the main s-process: their sensitivity to α-induced reactions on 13C and 22Ne and to the uncertainties of the nuclear network
This paper provides a detailed analysis of the main component of the slow neutron capture process(thes-process),whichaccountsforthesolarabundances ofhalfofthenucleiwith90 A 208. We examine the impact
A cautionary tale: The Coulomb modified ANC for the 1/2+2 state in 17O
• Physics
• 2018
Abstract.We discuss the impact of the uncertainty ($\pm 8$±8 keV) in the excitation energy of the astrophysically important 6.356 MeV $1/2^{+}_{2}$1/22+ state of 17O on the precision with which the
The Study of Key Reactions Shaping the Post-Main Sequence Evolution of Massive Stars in Underground Facilities
• Frontiers in Astronomy and Space Sciences
• 2020
The chemical evolution of the Universe and several phases of stellar life are regulated by minute nuclear reactions. The key point for each of these reactions is the value of cross-sections at the
Characterization of the LUNA neutron detector array for the measurement of the 13C(α, n)16O reaction
Abstract We introduce the LUNA neutron detector array developed for the investigation of the 13C( α , n )16O reaction towards its astrophysical s -process Gamow peak in the low-background environment
s process in low-mass asymptotic giant branch stars
• Physics
• 2006
Abstract The main component of the s process is produced by low mass stars ( 1.5 ⩽ M / M ⊙ ⩽ 3 ) , when they climb for the second time the red giant branch and experience a series of He shell flashes
The Importance of the 13C(α,n)16O Reaction in Asymptotic Giant Branch Stars
I will present a theoretical sensitivity study, carried out with the FUNS evolutionary stellar code, to evaluate the effects induced on the s-process nucleosynthesis by variations of the
EVOLUTION AND NUCLEOSYNTHESIS IN LOW-MASS ASYMPTOTIC GIANT BRANCH STARS. II. NEUTRON CAPTURE AND THE s-PROCESS
We present a new analysis of neutron capture occurring in low-mass asymptotic giant branch (AGB) stars suffering recurrent thermal pulses. We use dedicated evolutionary models for stars of initial
The 25Mg(p,g)Al reaction at low astrophysical energies
In the present work we report on a new measurement of resonance strengths ! in the reaction 25 Mg(p,) 26 Al at Ecm = 92 and 189 keV. This study was performed at the LUNA facility in the Gran Sasso