Suppression of the stellar enhancement factor and the reaction<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mmultiscripts><mml:mi mathvariant="normal">Rb</mml:mi><mml:mprescripts /><mml:none /><mml:mrow><mml:mn>85</mml:mn></mml:mrow></mml:mmultiscripts><mml:mrow><mml:mo stretchy="false">(</mml:mo><mml:mi>p</mml:mi><mml:mo>,</mml:mo><mml:mi>n</mml:mi><mml:mo stretchy="false">)</mml:mo></mml:mrow><mml:mmultiscripts><mml:mi mathvariant="normal">Sr</mml:mi><mml:mprescripts /><m

Rauscher, T.; Kiss, G. G.; Gyuerky, Gy.; Simón, A.; Fueloep, Zs.; Somorjai, E.

doi:10.1103/physrevc.80.035801

Cited by 46 publications

(50 citation statements)

References 32 publications

(53 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…[55] slightly changed the energy dependence but did not affect the magnitude of the cross section significantly. Recently, a modification of the imaginary part of the JLM potential was suggested to explain the energy dependence of low-energy (p,γ) data [34,[56][57][58]. Again, the impact here is negligible and it cannot account for the discrepancy of a factor of two.…”

Section: Implications For Astrophysical Proton Capture Onmentioning

confidence: 90%

Investigation of the reaction74Ge(p,γ)75
Sauerwein
¹
,
Endres
²
,
Netterdon
³

et al. 2012
Phys. Rev. C
Self Cite
36
4
40
0
View full text Add to dashboard Cite

Background: Astrophysical models studying the origin of the neutron-deficient p nuclides require the knowledge of proton capture cross sections at low energy. The production site of the p nuclei is still under discussion but a firm basis of nuclear reaction rates is required to address the astrophysical uncertainties. Data at astrophysically relevant interaction energies are scarce. Problems with the prediction of charged particle capture cross sections at low energy were found in the comparisons between previous data and calculations in the Hauser-Feshbach statistical model of compound reactions.Purpose: A measurement of 74 Ge(p,γ) 75 As at low proton energies, inside the astrophysically relevant energy region, is important in several respects. The reaction is directly important as it is a bottleneck in the reaction flow which produces the lightest p nucleus 74 Se. It is also an important addition to the data set required to test reaction-rate predictions and to allow an improvement in the global p+nucleus optical potential required in such calculations.Method: An in-beam experiment was performed, making it possible to measure in the range 2.1 ≤ Ep ≤ 3.7 MeV, which is for the most part inside the astrophysically relevant energy window. Angular distributions of the γ-ray transitions were measured with high-purity germanium detectors at eight angles relative to the beam axis. In addition to the total cross sections, partial cross sections for the direct population of twelve levels were determined. Results:The resulting cross sections were compared to Hauser-Feshbach calculations using the code SMARAGD. Only a constant renormalization factor of the calculated proton widths allowed a good reproduction of both total and partial cross sections. The accuracy of the calculation made it possible to check the spin assignment of some states in 75 As. In the case of the 1075 keV state, a double state with spins and parities of 3/2 − and 5/2 − is needed to explain the experimental partial cross sections. A change in parity from 5/2 + to 5/2 − is required for the state at 401 keV. Furthermore, in the case of 74 Ge, studying the combination of total and partial cross sections made it possible to test the γ width, which is essential in the calculation of the astrophysical 74 As(n,γ) 75 As rate. Conclusions:Between data and statistical model prediction a factor of about two was found. Nevertheless, the improved astrophysical reaction rate of 74 Ge(p,γ) (and its reverse reaction) is only 28% larger than the previous standard rate. The prediction of the 74 As(n,γ) 75 As rate (and its reverse) was confirmed, the newly calculated rate differs only by a few percent from the previous prediction. The in-beam method with high efficiency detectors proved to be a powerful tool for studies in nuclear astrophysics and nuclear structure.

show abstract

Section: Implications For Astrophysical Proton Capture Onmentioning

confidence: 90%

Investigation of the reaction74Ge(p,γ)75
Sauerwein
¹
,
Endres
²
,
Netterdon
³

et al. 2012
Phys. Rev. C
Self Cite
36
4
40
0
View full text Add to dashboard Cite

show abstract

“…However, by using the detailed balance theorem, information on the photodisintegration cross sections can be obtained from the experimental study of the inverse capture reactions. 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.…”

Section: A the Astrophysical γ Processmentioning

confidence: 99%

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

et al. 2013

Self Cite

View full text Add to dashboard Cite

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.

show abstract

“…Alternatively, the (γ ,α) rates can be determined experimentally by measuring the inverse (α,γ ) reaction cross section and converting the results by using the detailed balance theorem. 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
Self Cite

View full text Add to dashboard Cite

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).

show abstract

Suppression of the stellar enhancement factor and the reactionRb85(p,n)Sr

Cited by 46 publications

References 32 publications

Investigation of the reaction74Ge(p,γ)75
Sauerwein
¹
,
Endres
²
,
Netterdon
³

et al. 2012
Phys. Rev. C
Self Cite
36
4
40
0
View full text Add to dashboard Cite

Investigation of the reaction74Ge(p,γ)75
Sauerwein
¹
,
Endres
²
,
Netterdon
³

et al. 2012
Phys. Rev. C
Self Cite
36
4
40
0
View full text Add to dashboard Cite

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

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

et al. 2011
Phys. Rev. C
Self Cite

Contact Info

Product

Resources

About

Suppression of the stellar enhancement factor and the reactionRb85(p,n)Sr

Cited by 46 publications

References 32 publications

Investigation of the reaction74Ge(p,γ)75Sauerwein1, Endres2, Netterdon3 et al. 2012Phys. Rev. CSelf Cite364400View full textAdd to dashboardCite

Investigation of the reaction74Ge(p,γ)75Sauerwein1, Endres2, Netterdon3 et al. 2012Phys. Rev. CSelf Cite364400View full textAdd to dashboardCite

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

Cd110,116(α,α)Kiss1, Mohr2, Fülöp3 et al. 2011Phys. Rev. CSelf Cite

Contact Info

Product

Resources

About

Investigation of the reaction74Ge(p,γ)75
Sauerwein
¹
,
Endres
²
,
Netterdon
³

et al. 2012
Phys. Rev. C
Self Cite
36
4
40
0
View full text Add to dashboard Cite

Investigation of the reaction74Ge(p,γ)75
Sauerwein
¹
,
Endres
²
,
Netterdon
³

et al. 2012
Phys. Rev. C
Self Cite
36
4
40
0
View full text Add to dashboard Cite

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

et al. 2011
Phys. Rev. C
Self Cite