A direct measurement of the 17O(α,γ)21Ne reaction in inverse kinematics and its impact on heavy element production

Taggart, M.P.; Akers, C.; Laird, A. M.; Hager, U.; Ruiz, C.; Hutcheon, D. A.; Bentley, M. A.; Brown, J. R.; Buchmann, L.; Chen, A.A.; Chen, J.; Chipps, K. A.; Choplin, Arthur; D’Auria, J.M.; Davids, B.; Davis, C. A.; Diget, C. Aa.; Erikson, L.; Fallis, J.; Fox, S. P.; Frischknecht, U.; Fulton, B. R.; Galinski, N.; Greife, U.; Hirschi, Raphaël; Howell, Debra; Martin, L.; Mountford, David; Murphy, A. St. J.; Ottewell, D.; Pignatari, M.; Reeve, S.; Ruprecht, G.; Sjue, Sky; Veloce, L. M.; Williams, M.

doi:10.1016/j.physletb.2019.134894

Cited by 8 publications

(32 citation statements)

References 25 publications

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“…The red curve (label bg13) is the recommended rate of Best et al (2013). The green curve (label ta19) is the experimental lower limit from Taggart et al (2019). The shaded area indicates the approximate range of temperatures in the helium-burning core of massive stars.…”

Section: T [K]mentioning

confidence: 99%

“…In one case (models B), we used the rate from Best et al (2013) divided by 10 instead of the original rate from Best et al (2013). In a second case (models C) we adopted the lower limit from Taggart et al (2019) instead of Best et al (2013). Although theoretical and experimental works were carried out to study this rate (Descouvemont 1993;Best et al 2011Best et al , 2013Taggart et al 2019), significant uncertainties still remain in the temperature range of interest for the s-process.…”

Section: Stellar Evolution Modelsmentioning

confidence: 99%

“…In a second case (models C) we adopted the lower limit from Taggart et al (2019) instead of Best et al (2013). Although theoretical and experimental works were carried out to study this rate (Descouvemont 1993;Best et al 2011Best et al , 2013Taggart et al 2019), significant uncertainties still remain in the temperature range of interest for the s-process. The uncertainty on this rate was shown to dramatically affect the s-process efficiency in rotating massive stars (e.g.…”

Section: Stellar Evolution Modelsmentioning

confidence: 99%

“…The uncertainty on this rate was shown to dramatically affect the s-process efficiency in rotating massive stars (e.g. Taggart et al 2019). A low 17 O(α,γ) 21 Ne rate enhances the s-process efficiency because in this case, the competing 17 O(α,n) 20 Ne reaction becomes dominant and recycles neutrons (more details in Sect.…”

Section: Stellar Evolution Modelsmentioning

confidence: 99%

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Thep-process in exploding rotating massive stars

Choplin

Goriely

Hirschi

et al. 2022

A&A

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Context. The p-process nucleosynthesis can explain proton-rich isotopes that are heavier than iron, which are observed in the Solar System, but discrepancies still persist (e.g. for the Mo and Ru p-isotopes), and some important questions concerning the astrophysical site(s) of the p-process remain unanswered. Aims. We investigate how the p-process operates in exploding rotating massive stars that have experienced an enhanced s-process nucleosynthesis during their life through rotational mixing.Methods. With the Geneva stellar evolution code, we computed 25 M stellar models at a metallicity of Z = 10 −3 with different initial rotation velocities and rates for the still largely uncertain 17 O(α,γ) 21 Ne reaction. The nucleosynthesis calculation, followed with a network of 737 isotopes, was coupled to stellar evolution, and the p-process nucleosynthesis was calculated in post-processing during both the final evolutionary stages and spherical explosions of various energies. The explosions were modelled with a relativistic hydrodynamical code. Results. In our models, the p-nuclides are mainly synthesized during the explosion, but not much during the ultimate hydrostatic burning stages. The p-process yields mostly depend on the initial number of trans-iron seeds, which in turn depend on the initial rotation rate. We found that the impact of rotation on the p-process is comparable to the impact of rotation on the s-process. From no to fast rotation, the s-process yields of nuclides with mass number A < 140 increase by 3 − 4 dex, and so do the p-process yields. Fast rotation with a lower 17 O(α, γ) rate significantly produces s-and p-nuclides with A ≥ 140. The dependence of the p-process yields on the explosion energy is very weak. Conclusions. Our results suggest that the contribution of core-collapse supernovae from massive stars to the solar (and Galactic) pnuclei has been underestimated in the past, and more specifically, that the contribution from massive stars with sub-solar metallicities may even dominate. A more detailed study including stellar models with a wide range of masses and metallicities remains to be performed, together with a quantitative analysis that is based on the chemical evolution of the Galaxy.

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Section: T [K]mentioning

confidence: 99%

Section: Stellar Evolution Modelsmentioning

confidence: 99%

Section: Stellar Evolution Modelsmentioning

confidence: 99%

Section: Stellar Evolution Modelsmentioning

confidence: 99%

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Thep-process in exploding rotating massive stars

Choplin

Goriely

Hirschi

et al. 2022

A&A

Self Cite

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“…O N e   reaction has been performed at the DRAGON facility, at the TRIUMF laboratory, Canada [9]. At this laboratory, the 22.…”

Section: ( )mentioning

confidence: 99%

Polarization Effects in the Reaction d+eˉ → d+eˉ

2021

EEJP

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The differential cross section and polarization observables for the elastic reaction induced by deuteron scattering off electrons at rest, are calculated in the one-photon-exchange approximation. The following polarization observables were calculated: 1- the analyzing powers (asymmetries) due to the tensor polarization of the deuteron beam, 2 - the spin correlation coefficients caused by the arbitrarily polarized electron target and the vector polarized deuteron beam, 3 - the coefficients of the polarization transfer from the arbitrarily polarized target electron to the recoil electrons. The differential cross section and polarization observables have been expressed in terms of the deuteron electromagnetic form factors: (charge monopole), (magnetic dipole) and (charge quadrupole). Numerical estimations are given for the analyzing powers (asymmetries) due to the tensor polarization of the deuteron beam. They are calculated as functions of the deuteron beam energy for some values of the scattering angle (the angle between the deuteron beam and the recoil electron momenta). For the numerical calculation we use the existing phenomenological parametrization of the deuteron electromagnetic form factors. It turns out that the analyzing powers (asymmetries) are increasing with the growth of the deuteron beam energy and they have appreciable sensitivity to the value of the scattering angle. The specific interest of this reaction is to investigate the possibility to use this reaction for the measurement of the polarization of the high energy deuteron beams.

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Slow Neutron-Capture Process in Evolved Stars

Hirschi

2023

Handbook of Nuclear Physics

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A direct measurement of the 17O(α,γ)21Ne reaction in inverse kinematics and its impact on heavy element production

Cited by 8 publications

References 25 publications

Thep-process in exploding rotating massive stars

Thep-process in exploding rotating massive stars

Polarization Effects in the Reaction d+eˉ → d+eˉ

Slow Neutron-Capture Process in Evolved Stars

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