Astrophysical<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mrow><mml:mi>S</mml:mi></mml:mrow></mml:math>factor for α-capture on<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mmultiscripts><mml:mi mathvariant="normal">Sn</mml:mi><mml:mprescripts /><mml:none /><mml:mrow><mml:mn>112</mml:mn></mml:mrow></mml:mmultiscripts></mml:math>in the<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mrow><mml:mi>p</mml:mi></mml:m

Özkan, N.; Efe, G.; Güray, R. T.; Palumbo, A.; Görres, J.; Lee, Hye Young; Lamm, L. O.; Rapp, W.; Stech, E.; Wiescher, M.; Gyürky, György; Fülöp, Zs.; Somorjai, E.

doi:10.1103/physrevc.75.025801

Cited by 63 publications

(97 citation statements)

References 35 publications

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“…As a result, in order to avoid any question concerning the remaining parameters largely needed within statistical model calculations, a DFM-based semi-microscopic analysis of only α-particle elastic scattering on A ∼100 nuclei at energies from ∼14 to 32 MeV has been carried out [12]. The use of this potential at even lower energies has provided a suitable description of the (α, n) reaction cross sections for lighter target nuclei with A≤54 [13], while it has led to a major overestimation of (α, γ) reaction cross sections for 106 Cd [14] and 112 Sn [15]. Better results have been provided in the later cases by either the well-known mass-and energy-independent fourparameter global potential of McFadden and Satchler [16] obtained by analysis of 26 MeV α-particle elastic scattering, or with the potential of Refs.…”

Section: Introductionmentioning

confidence: 99%

Complementary optical-potential analysis of -particle elastic scattering and induced reactions at low energies

Avrigeanu

Obreja

Román

et al. 2009

Atomic Data and Nuclear Data Tables

175

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A previously derived semi-microscopic analysis based on the Double Folding Model, for α-particle elastic scattering on A ∼100 nuclei at energies below 32 MeV, is extended to medium mass A ∼50-120 nuclei and energies from ∼13 to 50 MeV. The energy-dependent phenomenological imaginary part for this semi-microscopic optical model potential was obtained including the dispersive correction to the microscopic real potential, and used within a concurrent phenomenological analysis of the same data basis. A regional parameter set for low-energy α-particles entirely based on elastic-scattering data analysis was also obtained for nuclei within the above-mentioned mass and energy ranges. Then, an ultimate assessment of (α, γ), (α, n) and (α, p) reaction cross sections concerned target nuclei from 45 Sc to 118 Sn and incident energies below ∼12 MeV. The former diffuseness of the real part of optical potential as well as the surface imaginary-potential depth have been found responsible for the actual difficulties in the description of these data, and modified in order to obtain an optical potential which describe equally well both the low energy elastic-scattering and induced-reaction data of α-particles.

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Section: Introductionmentioning

confidence: 99%

Complementary optical-potential analysis of -particle elastic scattering and induced reactions at low energies

Avrigeanu

Obreja

Román

et al. 2009

Atomic Data and Nuclear Data Tables

175

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“…These rates are typically calculated with the statistical Hauser Feshbach (HF) model [4] in a reaction network involving thousands of nuclei. However, the HF model predictions are in disagreement with measured (α,γ) cross sections at low energies [5,6]. To improve the reliability of the HF reaction rates, experimental verifications and constraints are needed.…”

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confidence: 99%

“…In recent years, a number of α-beam activation measurements have been conducted for targets relevant to pprocess [5][6][7][8][9][10][11][12][13]. Cross sections of the corresponding (α,x) reactions were measured at, or close to, the astrophysically relevant energy.…”

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confidence: 99%

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Measurement of120Te(α,n) cross sections relevant to the astrophysicalp

et al. 2012

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The cross section calculation of 112Sn(α,γ)116Te reaction with different nuclear models at the astrophysical energy range

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2017

NUCL SCI TECH

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The theoretical cross section calculations for the astrophysical p process are needed because the most of the related reactions are technically very difficult to be measured in the laboratory. Even if the reaction was measured, most of the measured reactions have been carried out at the higher energy range from the astrophysical energies. Therefore, almost all cross sections needed for p process simulation has to be theoretically calculated or extrapolated to the astrophysical energies. The 112 Sn(α,γ) 116 Te is an important reaction for the p process nucleosynthesis. The theoretical cross section of the 112 Sn(α,γ) 116 Te reaction was investigated for different global optical model potentials, level density and strength function models at the astrophysically interested energies. Astrophysical S factors were calculated and compared with experimental data available in EXFOR database. The calculation with the optical model potential of the dispersive model by Demetriou et al., and Back-shifted Fermi gas level density model and Brink-Axel Lorentzian strength function model best served to reproduce experimental results at astrophysically relevant energy region. The reaction rates were calculated with these model parameters at the p process temperature and compared with the current version of the reaction rate library Reaclib and Starlib.

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AstrophysicalSfactor for α-capture onSn112in thep

Cited by 63 publications

References 35 publications

Complementary optical-potential analysis of -particle elastic scattering and induced reactions at low energies

Complementary optical-potential analysis of -particle elastic scattering and induced reactions at low energies

Measurement of120Te(α,n) cross sections relevant to the astrophysicalp

The cross section calculation of 112Sn(α,γ)116Te reaction with different nuclear models at the astrophysical energy range

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