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<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mrow><mml:mi>α</mml:mi></mml:mrow></mml:math>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>117</mml:mn></mml:mrow></mml:mmultiscripts></mml

Căta-Danil, I.; Filipescu, D.; Ivaşcu, M.; Bucurescu, D.; Zamfir, N. V.; Glodariu, T.; Stroe, L.; Cǎta-Danil, G.; Mihai, C.; Suliman, G.; Sava, T.

doi:10.1103/physrevc.78.035803

Cited by 32 publications

(36 citation statements)

References 25 publications

(25 reference statements)

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“…This approach provides more relevant astrophysical information than the direct study of the γ -induced reactions since often the influence of thermally excited states is smaller in this direction, compared to photon-induced reactions [16,[22][23][24]. In recent years several α-capture cross sections have been measured using the well known activation technique [25][26][27][28][29][30][31][32][33], and the results were compared with the H-F predictions. In general, it was found that the H-F cross sections are very sensitive to the choice of the α + nucleus OMP, in particular at energies significantly below the Coulomb barrier, which is the most relevant energy range for the calculation of stellar reaction rates.…”

Section: A the Astrophysical γ Processmentioning

confidence: 99%

High precision113In(α,α)113In elastic scattering at energies near the Coulomb barrie

et al. 2013

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Background:The γ process in supernova explosions is thought to explain the origin of proton-rich isotopes between Se and Hg, the so-called p nuclei. The majority of the reaction rates for γ process reaction network studies have to be predicted in Hauser-Feshbach statistical model calculations using global optical potential parametrizations. While the nucleon + nucleus optical potential is fairly well known, for the α + nucleus optical potential several different parametrizations exist and large deviations are found between the predictions calculated using different parameter sets. Purpose: By the measurement of elastic α-scattering angular distributions at energies around the Coulomb barrier a comprehensive test for the different global α + nucleus optical potential parameter sets is provided. Methods: Between 20 • and 175 • complete elastic alpha scattering angular distributions were measured on the 113 In p nucleus with high precision at E c.m. = 15.59 and 18.82 MeV. Results: The elastic scattering cross sections of the 113 In(α,α) 113 In reaction were measured for the first time at energies close to the astrophysically relevant energy region. The high precision experimental data were used to evaluate the predictions of the recent global and regional α + nucleus optical potentials. Parameters for a local α + nucleus optical potential were derived from the measured angular distributions. Conclusions: Predictions for the reaction cross sections of 113 In(α, γ ) 117 Sb and 113 In(α,n) 116 Sb at astrophysically relevant energies were given using the global and local optical potential parametrizations.

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Section: A the Astrophysical γ Processmentioning

confidence: 99%

High precision113In(α,α)113In elastic scattering at energies near the Coulomb barrie

et al. 2013

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“…In this direction the influence of thermally excited states remains relatively small [7,8]. In recent years a range of (α,γ ) reaction cross sections on 70 Ge, 96 Ru, 106 Cd, 112,117 Sn, 113 In, 144 Sm, 151 Eu, and 169 Tm has been measured using the activation method, and the results have been compared with model predictions [9][10][11][12][13][14][15][16][17].…”

Section: Introductionmentioning

confidence: 99%

Cd110,116(α,α)
Kiss
¹
,
Mohr
²
,
Fülöp
³

et al. 2011
Phys. Rev. C

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The elastic scattering cross sections for the reactions 110,116 Cd(α,α) 110,116 Cd at energies above and below the Coulomb barrier are presented to provide a sensitive test for the α-nucleus optical potential parameter sets. Additional constraints for the optical potential are taken from the analysis of elastic scattering excitation functions at backward angles which are available in literature. Moreover, the variation of the elastic α scattering cross sections along the Z = 48 isotopic and N = 62 isotonic chain is investigated by the study of the ratios of the 106,110,116 Cd(α,α) 106,110,116 Cd scattering cross sections at E cm ≈ 15.6 and 18.8 MeV and the ratio of the 110 Cd(α,α) 110 Cd and 112 Sn(α,α) 112 Sn reaction cross sections at E cm ≈ 18.8 MeV, respectively. These ratios are sensitive probes for the α-nucleus optical potential parametrizations. The potentials under study are a basic prerequisite for the prediction of α-induced reaction cross sections (e.g., for the calculation of stellar reaction rates in the astrophysical p or γ process).

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“…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.…”

mentioning

confidence: 99%