Alpha induced reaction cross section measurements on 162Er for the astrophysical γ process

Kiss, G.; Szücs, T.; Rauscher, T.; Török, Zsófia; Fülöp, Zs.; Gyürky, Gy.; Halász, Z.; Somorjai, E.

doi:10.1016/j.physletb.2014.06.011

Cited by 38 publications

(58 citation statements)

References 33 publications

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“…It was found that the experimental cross sections for both reactions are smaller than the ones predicted by the reaction model which has been used in previous γ-process studies. This is in line with the findings of previous (α,γ) and (α,n) experiments on other p nuclei, which also showed smaller cross sections than predicted (see [15,20,23] and references in [32]). …”

Section: Conclusion and Summarysupporting

confidence: 92%

“…An experimental check of the theoretical cross sections is therefore important to examine one possible reason of the deficiencies. This need triggered huge experimental work in the last decade on studying reactions relevant for the γ process (see the references in the review paper [6] and some of the most recent studies [14][15][16][17][18][19][20][21][22][23][24][25][26][27][28][29][30][31]). …”

Section: Introductionmentioning

confidence: 99%

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Experimental study of the astrophysicalγ-process reactionXe124(α,γ)Ba
Halász
¹
,
Somorjai
²
,
Gyürky
³

et al. 2016
Phys. Rev. C
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16
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0
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Background: The synthesis of heavy, proton rich isotopes in the astrophysical γ process proceeds through photodisintegration reactions. For the improved understanding of the process, the rates of the involved nuclear reactions must be known. The reaction 128 Ba(γ,α) 124 Xe was found to affect the abundance of the p nucleus 124 Xe in previous rate variation studies.Purpose: Since the stellar rate for this reaction cannot be determined by a measurement directly, the aim of the present work was to measure the cross section of the inverse 124 Xe(α,γ) 128 Ba reaction and to compare the results with statistical model predictions used in astrophysical networks. Modified nuclear input can then be used to provide an improved stellar reaction rate. Of great importance is the fact that data below the (α,n) threshold was obtained. Studying simultaneously the 124 Xe(α,n) 127 Ba reaction channel at higher energy allowed to further identify the source of a discrepancy between data and prediction.Method: The 124 Xe(α,γ) 128 Ba and 124 Xe(α,n) 127 Ba cross sections were measured with the activation method using a thin window 124 Xe gas cell and an α beam from a cyclotron accelerator. The studied energy range was between Eα = 11 and 15 MeV close above the astrophysically relevant energy range. Results:The obtained cross sections are compared with Hauser-Feshbach statistical model calculations. The experimental cross sections are smaller than standard predictions previously used in astrophysical calculations. As dominating source of the difference, the theoretical α width was identified. The experimental data suggest an α width lower by at least a factor of 0.125 in the astrophysically important energy range.Conclusions: An upper limit for the 128 Ba(γ,α) 124 Xe stellar rate was inferred from our measurement. The impact of this rate and lower rates was studied in two different models for core-collapse supernova explosions of 25 M⊙ stars. A significant contribution to the 124 Xe abundance via this reaction path would only be possible when the rate was increased above the previous standard value. Since the experimental data rule this out, they also demonstrate the closure of this production path.

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Section: Conclusion and Summarysupporting

confidence: 92%

Section: Introductionmentioning

confidence: 99%

Experimental study of the astrophysicalγ-process reactionXe124(α,γ)Ba
Halász
¹
,
Somorjai
²
,
Gyürky
³

et al. 2016
Phys. Rev. C
Self Cite
16
0
17
0
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“…The more recent (α, x) reaction data concern mainly heavier target nuclei and incident energies well below B [4][5][6][7][8][9][10][11][12][13][14] (Fig. 1).…”

Section: (α X) Reaction Data Analysismentioning

confidence: 99%

“…Thus, while the use of this potential led to description of some new data almost as well as local potentials [3-7, 9, 17] or showing the best agreement of global potentials [1,2,[18][19][20], underestimation of newer data [8,[10][11][12][13][14] was also found. Hence a revision of this OMP [16] became desirable and forms the object of the present work.…”

Section: Introductionmentioning

confidence: 99%

Further explorations of theα-particle optical model potential at low energies for the mass rangeA≈45–209

2014

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The recent high-precision measurements of α-particle induced reaction data below the Coulomb barrier (B) make possible the understanding of limits and possible improvement of a previous optical model potential (OMP) for α-particles on nuclei within the mass number range 45≤A≤209 [M. Avrigeanu et al., Phys. Rev. C 82, 014606 (2010)]. An updated version of this potential is given in the present work concerning mainly an increased surface imaginary potential depth well below B for A>130. Moreover, underestimation of reaction cross sections for well-deformed nuclei is removed by using ∼7% larger radius for the surface imaginary part of this spherical OMP. Improved input parameters based on recent independent data, particularly γ-ray strength functions, but no empirical rescaling factor of the γ and/or neutron widths have been involved within statistical model calculation of the corresponding (α, x) reaction cross sections.

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“…Although the descent of the abundances of the elements is generally good understood, significant uncertainties still exist [3]. Therefore, recently (α,n) and (α,γ) reaction cross-sections in low energies are measured by several authors [4][5][6][7][8][9]. The importance of alpha capture cross sections for different mass regions to test the theoretical models is well known [10].…”

Section: " # "mentioning

confidence: 99%

Theoretical investigation of cross sections and astrophysical S-factors for the⁹²Mo(α,n)⁹⁵Ru and⁹⁴Mo(α,n)⁹⁷Ru reactions

2016

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Abstract.Molybdenum is commonly applied as a constructive material in different types of nuclear reactors. The cross sections of the 92 Mo(α,n) 95 Ru and 94 Mo(α,n) 97 Ru reactions have been calculated at 5-20 MeV energy ranges. In theoretical calculations, the TALYS1.6 and NON-SMOKER codes were used. Also the astrophysical S-factors were calculated. Results of our calculations were checked to the experimental data obtained from EXFOR database.

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Alpha induced reaction cross section measurements on 162Er for the astrophysical γ process

Cited by 38 publications

References 33 publications

Experimental study of the astrophysicalγ-process reactionXe124(α,γ)Ba
Halász
¹
,
Somorjai
²
,
Gyürky
³

et al. 2016
Phys. Rev. C
Self Cite
16
0
17
0
View full text Add to dashboard Cite

Experimental study of the astrophysicalγ-process reactionXe124(α,γ)Ba
Halász
¹
,
Somorjai
²
,
Gyürky
³

et al. 2016
Phys. Rev. C
Self Cite
16
0
17
0
View full text Add to dashboard Cite

Further explorations of theα-particle optical model potential at low energies for the mass rangeA≈45–209

Theoretical investigation of cross sections and astrophysical S-factors for the⁹²Mo(α,n)⁹⁵Ru and⁹⁴Mo(α,n)⁹⁷Ru reactions

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Alpha induced reaction cross section measurements on 162Er for the astrophysical γ process

Cited by 38 publications

References 33 publications

Experimental study of the astrophysicalγ-process reactionXe124(α,γ)BaHalász1, Somorjai2, Gyürky3 et al. 2016Phys. Rev. CSelf Cite160170View full textAdd to dashboardCite

Experimental study of the astrophysicalγ-process reactionXe124(α,γ)BaHalász1, Somorjai2, Gyürky3 et al. 2016Phys. Rev. CSelf Cite160170View full textAdd to dashboardCite

Further explorations of theα-particle optical model potential at low energies for the mass rangeA≈45–209

Theoretical investigation of cross sections and astrophysical S-factors for the92Mo(α,n)95Ru and94Mo(α,n)97Ru reactions

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Product

Resources

About

Experimental study of the astrophysicalγ-process reactionXe124(α,γ)Ba
Halász
¹
,
Somorjai
²
,
Gyürky
³

et al. 2016
Phys. Rev. C
Self Cite
16
0
17
0
View full text Add to dashboard Cite

Experimental study of the astrophysicalγ-process reactionXe124(α,γ)Ba
Halász
¹
,
Somorjai
²
,
Gyürky
³

et al. 2016
Phys. Rev. C
Self Cite
16
0
17
0
View full text Add to dashboard Cite

Theoretical investigation of cross sections and astrophysical S-factors for the⁹²Mo(α,n)⁹⁵Ru and⁹⁴Mo(α,n)⁹⁷Ru reactions