Total Neutron Yield from the (<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mi>α</mml:mi></mml:math>,<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mi>n</mml:mi></mml:math>) Reaction on<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mrow><mml:mmultiscripts><mml:mrow><mml:mi mathvariant="normal">Ne</mml:mi></mml:mrow><mml:mprescripts /><mml:mrow /><mml:mrow><mml:mn>2</mml:mn><mml:mn>1</mml:mn><mml:mo>,</mml:mo><m

Haas, F.; Bair, J.K.

doi:10.1103/physrevc.7.2432

Cited by 29 publications

(33 citation statements)

References 7 publications

Supporting

Mentioning

Contrasting

Unclassified

Order By: Relevance

“…Considerable efforts have been made in the past to perform direct measurements of the 22 Ne(α,n) 25 Mg ( [43], [44], [45], [46], [47] and [48]) and the 22 Ne(α, γ) 26 Mg ( [47] and [49]) reactions. Unfortunately, in the astrophysical region of interest, α-penetrability is largely suppressed by the Coulomb barrier and very difficult to measure because of the cosmic and beam-induced background in the detector materials.…”

Section: Level Density and Alpha Cluster Structurementioning

confidence: 99%

Probing astrophysically important states in theMg26nucleus to study neutron sources for thesprocess

et al. 2016

View full text Add to dashboard Cite

Section: Level Density and Alpha Cluster Structurementioning

confidence: 99%

Probing astrophysically important states in theMg26nucleus to study neutron sources for thesprocess

et al. 2016

View full text Add to dashboard Cite

“…The reduced cross sections σ red for 21 Ne from the experimental 21 Ne(α,n) 24 Mg data of [147,156,157] are shown in Fig. 61.…”

Section: 32mentioning

confidence: 99%

“…60 24 Na reactions. The experimental data have been taken from [147,156,157]. Further discussion see text.…”

Section: 32mentioning

confidence: 99%

See 1 more Smart Citation

Cross sections of α-induced reactions for targets with masses A ≈ 20–50 at low energies

Mohr

2015

Eur. Phys. J. A

100

View full text Add to dashboard Cite

Abstract. A simple reduction scheme using so-called reduced energies E red and reduced cross sections σ red allows the comparison of heavy-ion induced reaction cross sections for a broad range of masses of projectile and target and over a wide energy range. A global behavior has been found for strongly bound projectiles whereas much larger reduced cross sections have been observed for weakly bound and halo projectiles. It has been shown that this simple reduction scheme works also well for α-particle induced reactions on heavy target nuclei, but very recently significant deviations have been seen for α+ 33 S and α+ 23 Na. Motivated by these unexpected discrepancies, the present study analyses α-induced reaction cross sections for targets with masses A ≈ 20 − 50. The study shows that the experimental data for α-induced reactions on nuclei with A ≈ 20 − 50 deviate slightly from the global behavior of reduced cross sections. However, in general the deviations evolve smoothly towards lower masses. The only significant outliers are the recent data for 33 S and 23 Na which are far above the general systematics, and some very old data may indicate that 36 Ar and 40 Ar are below the general trend. As expected, also the doubly-magic 40 Ca nucleus lies slightly below the results for its neighboring nuclei. Overall, the experimental data are nicely reproduced by a statistical model calculation utilizing the simple α-nucleus potential by McFadden and Satchler. Simultaneously with the deviation of reduced cross sections σ red from the general behavior, the outliers 23 Na, 33 S, 36 Ar, and 40 Ar also show significant disagreement between experiment and statistical model calculation.PACS. 25.55.-e 3H-, 3He-, and 4He-induced reactions -24.10.Pa Thermal and statistical models

show abstract

“…Several experiments have been performed making direct measurements of the 22 Ne(α,n) 25 Mg [9][10][11][12][13][14] and 22 Ne(α,γ ) 26 Mg [13,15] reactions. These measurements have been unable to access the astrophysical energy region because of the relatively high α penetrability through the Coulomb barrier as well as unwanted background from cosmic rays and beam induced reactions.…”

Section: Introductionmentioning

confidence: 99%

Photoexcitation of astrophysically important states inMg26. II. Ground-state-transition partial widths

et al. 2010

View full text Add to dashboard Cite

The level structure of 26 Mg near the neutron-separation energy, which is of interest for s-process nucleosynthesis, was studied at the High Intensity Gamma-Ray Source of the Triangle Universities Nuclear Laboratory using the method of nuclear resonance fluorescence. A nearly monoenergetic and linearly polarized γ -ray beam was used to scan the excitation energy range from 10.5 to 11.7 MeV. For the five states observed, the total widths and partial widths are determined. Precise measurement of these widths is necessary for the prediction of neutron production for the s-process.

show abstract

Total Neutron Yield from the (α,n) Reaction onNe21,

Cited by 29 publications

References 7 publications

Probing astrophysically important states in theMg26nucleus to study neutron sources for thesprocess

Probing astrophysically important states in theMg26nucleus to study neutron sources for thesprocess

Cross sections of α-induced reactions for targets with masses A ≈ 20–50 at low energies

Photoexcitation of astrophysically important states inMg26. II. Ground-state-transition partial widths

Contact Info

Product

Resources

About