Uncertainty of the astrophysical 
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Mohr, P.

doi:10.1103/physrevc.96.045808

Cited by 9 publications

(7 citation statements)

References 42 publications

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“…Of course, such a statistical model approach can only be valid on average, and individual resonances in the 13 C(α,n) 16 O reaction may show a completely different decay branching. But it has been shown recently that a careful selection of TALYS parameters allows to reproduce (α,n) cross sections for intermediate [20,21] and even light nuclei [22], at least at energies E α above a few MeV. The calculated branching ratios b j as a function of energy E α are shown in Fig.…”

Section: Re-analysis Of the Har05 Datamentioning

confidence: 99%

Revised cross section of the C13(α, n)O16 react

Mohr

2018

Phys. Rev. C

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As suggested in a Comment by Peters, Phys. Rev. C 96, 029801 (2017), a correction is applied to the 13 C(α,n) 16 O data of Harissopulos et al., Phys. Rev. C 72, 062801(R) (2005). The correction refers to the energy-dependent efficiency of the neutron detector and appears only above the (α,n1) threshold of the 13 C(α,n) 16 O reaction at about Eα ≈ 5 MeV. The corrected data are lower than the original data by almost a factor of two. The correction method is verified using recent neutron spectroscopy data and data from the reverse 16 O(n,α) 13 C reaction.

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Section: Re-analysis Of the Har05 Datamentioning

confidence: 99%

Revised cross section of the C13(α, n)O16 react

Mohr

2018

Phys. Rev. C

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“…[7] (black dasheddotted line) and TALYS [15] (blue dashed line). For the TALYS calculations, the McFadden/Satchler alpha optical model potential has been used, which has been shown to be the best at reproducing the reaction cross sections for the mass range A = 20 − 50 [16] and below, including the 13 C(α,n) 16 O mirror reaction [17,18].…”

Section: Resultsmentioning

confidence: 99%

First direct measurement of the $^{13}$N($α$,$p$)$^{16}$O reaction relevant for core-collapse supernovae nucleosynthesis

Jayatissa,

Avila,

Rehm

et al. 2022

Preprint

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Understanding the explosion mechanism of a core-collapse supernova (CCSN) is important to accurately model CCSN scenarios for different progenitor stars using model-observation comparisons. The uncertainties of various nuclear reaction rates relevant for CCSN scenarios strongly affect the accuracy of these stellar models. Out of these reactions, the 13 N(α,p) 16 O reaction has been found to affect various stages of a CCSN at varying temperatures. This work presents the first direct measurement of the 13 N(α,p) 16 O reaction performed using a 34.6 MeV beam of radioactive 13 N ions and the active-target detector MUSIC (MUlti-Sampling Ionization Chamber) at Argonne National Laboratory. The resulting total 13 N(α,p) 16 O reaction cross sections from this measurement in the center-of-mass energy range of 3.26 -6.02 MeV are presented and compared with calculations using the Hauser-Feshbach formalism. Uncertainties in the reaction rate have been dramatically reduced at CCSN temperatures.

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“…A subsequent uncertainty analysis of the measured 17 O(α,n) 20 Ne excitation functions presented in the literature was performed by Mohr (2017), which raised some doubts about the consistency of the data presented in Best et al (2013) in comparison to historical literature. However, the study found the largest discrepancy was in the high-energy cross section affecting the reaction rate at temperatures above 1 GK.…”

Section: Existing Literature On 21 Ne Levelsmentioning

confidence: 99%

The impact of 17O + α reaction rate uncertainties on the s-process in rotating massive stars

Frost-Schenk

Adsley

Laird

et al. 2022

Monthly Notices of the Royal Astronomical Society

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Massive stars are crucial to galactic chemical evolution for elements heavier than iron. Their contribution at early times in the evolution of the Universe, however, is unclear due to poorly constrained nuclear reaction rates. The competing 17O(α, γ)21Ne and 17O(α, n)20Ne reactions strongly impact weak s-process yields from rotating massive stars at low metallicities. Abundant 16O absorbs neutrons, removing flux from the s-process, and producing 17O. The 17O(α, n)20Ne reaction releases neutrons, allowing continued s-process nucleosynthesis, if the 17O(α, γ)21Ne reaction is sufficiently weak. While published rates are available, they are based on limited indirect experimental data for the relevant temperatures and, more importantly, no uncertainties are provided. The available nuclear physics has been evaluated, and combined with data from a new study of astrophysically relevant 21Ne states using the 20Ne(d, p)21Ne reaction. Constraints are placed on the ratio of the (α, n)/(α, γ) reaction rates with uncertainties on the rates provided for the first time. The new rates favour the (α, n) reaction and suggest that the weak s-process in rotating low-metallicity stars is likely to continue up to barium and, within the computed uncertainties, even to lead.

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Uncertainty of the astrophysical O17,18(α,n)Ne20,21

Cited by 9 publications

References 42 publications

Revised cross section of the C13(α, n)O16 react

Revised cross section of the C13(α, n)O16 react

First direct measurement of the $^{13}$N($α$,$p$)$^{16}$O reaction relevant for core-collapse supernovae nucleosynthesis

The impact of 17O + α reaction rate uncertainties on the s-process in rotating massive stars

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