Thick-target measurements and astrophysical thermonuclear reaction rates: Proton-induced reactions

Roughton, N. A.; Fritts, M.R.; Peterson, R. J.; Zaidins, C.S.; Hansen, Carl J.

doi:10.1016/0092-640x(79)90004-4

Cited by 65 publications

(75 citation statements)

References 9 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…As a consequence, the cross section in the StM in Eq. (3) factorizes into a production cross section of the compound nucleus which is proportional to T α,0 , and a decay branching ratio b X = T X / i T i practi- 50 Cr(α,α) 50 Cr elastic scattering: experimental data [34] and a phase shift fit to determine the total reaction cross section σreac using the method from [35].…”

Section: Statistical Modelmentioning

confidence: 99%

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

Section: Statistical Modelmentioning

confidence: 99%

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

show abstract

“…The results of the most recent models seem to be roughly comparable. As far as experiment is concerned, we can also only cite a sampling of the many papers from a variety of sources, including Caltech (Zyskind et al, 1977), the University of Colorado (Roughton et al, 1979, Roughton et al, 1983, and the University of Melbourne (Sargood, 1982). Figure 13 shows an example of a phenomenon that Fowler and Caltech colleagues have named competition cusps.…”

Section: E Silicon Burningmentioning

confidence: 99%

Synthesis of the elements in stars: forty years of progress

et al. 1997

View full text Add to dashboard Cite

Forty years ago Burbidge, Burbidge, Fowler, and Hoyle combined what we would now call fragmentary evidence from nuclear physics, stellar evolution and the abundances of elements and isotopes in the solar system as well as a few stars into a synthesis of remarkable ingenuity. Their review provided a foundation for forty years of research in all of the aspects of low energy nuclear experiments and theory, stellar modeling over a wide range of mass and composition, and abundance studies of many hundreds of stars, many of which have shown distinct evidence of the processes suggested by B 2 FH. In this review we summarize progress in each of these fields with emphasis on the most recent developments. [S0034-6861(97)

show abstract

“…The resulting S(E)-factor in absolute units displayed as black diamonds obtained in [8] and the previous data sets [9] S(E)-factor shown as black stars.This S(E)-factor is compared with data from the ref [15] as blue circles, with the data from [14] corrected for the factor 1.83 as recommended in [15] and reported as red squares. Moreover thick-target data in [11] reported as purple circles, and recent works [12] and [13] S(E) -factors as green and grey triangles, respectively. R-matrix fit of the THM data is reported as red line the detected particles were processed by standard electronics and sent to the acquisition system for the on-line monitoring and data storage.…”

Section: Methodsmentioning

confidence: 70%

“…In order to study the 10 keV resonance the energy resolution effects and selection of the events of interest for the THM investigation have been carefully evaluated together with the corresponding uncertainties [9]. The THM astrophysical factor in absolute units has been obtained by normalization to direct data [11][12][13] in a energy range from 200 to 1200 keV. Thanks to this wide normalization range we are able to reach a very low normalization uncertainty (4%).…”

Section: Discussionmentioning

confidence: 99%

The ¹⁰B(p,α)⁷Be S(E)-factor from 5 keV to 1.5 MeV using the Trojan Horse Method

et al. 2017

View full text Add to dashboard Cite

Abstract. The 10 B(p,α) 7 Be reaction is the main responsible for the 10 B destruction in stellar interior [1]. In such environments this p-capture process occurs at a Gamow energy of 10 keV, and takes places mainly through a resonant state (Ex = 8.701 MeV) of the compound 11 C nucleus. Thus, a resonance right in the region of the Gamow peak is expected to significantly influence the behavior of the astrophysical S(E)-factor. The 10 B(p,α) 7 Be reaction was studied via the Trojan Horse Method (THM) applied to the 2 H( 10 B,α 7 Be)n in order to extract the astrophysical S(E)-factor in a wide energy range, from 5 keV to 1.5 MeV.

show abstract

Thick-target measurements and astrophysical thermonuclear reaction rates: Proton-induced reactions

Cited by 65 publications

References 9 publications

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

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

Synthesis of the elements in stars: forty years of progress

The ¹⁰B(p,α)⁷Be S(E)-factor from 5 keV to 1.5 MeV using the Trojan Horse Method

Contact Info

Product

Resources

About

Thick-target measurements and astrophysical thermonuclear reaction rates: Proton-induced reactions

Cited by 65 publications

References 9 publications

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

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

Synthesis of the elements in stars: forty years of progress

The 10B(p,α)7Be S(E)-factor from 5 keV to 1.5 MeV using the Trojan Horse Method

Contact Info

Product

Resources

About

The ¹⁰B(p,α)⁷Be S(E)-factor from 5 keV to 1.5 MeV using the Trojan Horse Method