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Ejnisman, R.; Goldman, I. D.; Krane, K. S.; Mohr, P.; Nakazawa, Yasuhiro; Norman, E. B.; Rauscher, T.; Reel, J.

doi:10.1103/physrevc.58.2531

Cited by 9 publications

(9 citation statements)

References 26 publications

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“…It was also used to extend calculations to intermediate and heavy target nuclei. 140,229,233,235,236,240,247,261,262,263,264,265,266,267,268 Other astrophysical calculations have not made use of the full DC equations but used simplifying assumptions. Resonant and DC rates on the proton-rich side based on hard sphere scattering wavefunctions in the entrance channel -with resonance properties, final states, and spectroscopic factors taken from shell model calculations -were provided for target nuclei with mass number 44 ≤Ã ≤ 63.…”

Section: T Rauschermentioning

confidence: 99%

The Path to Improved Reaction Rates for Astrophysics

Rauscher

2011

Int. J. Mod. Phys. E

144

337

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This review focuses on nuclear reactions in astrophysics and, more specifically, on reactions with light ions (nucleons and α particles) proceeding via the strong interaction. It is intended to present the basic definitions essential for studies in nuclear astrophysics, to point out the differences between nuclear reactions taking place in stars and in a terrestrial laboratory, and to illustrate some of the challenges to be faced in theoretical and experimental studies of those reactions. The discussion revolves around the relevant quantities for astrophysics, which are the astrophysical reaction rates. The sensitivity of the reaction rates to the uncertainties in the prediction of various nuclear properties is explored and some guidelines for experimentalists are also provided.Caminante, son tus huellas el camino, y nada más; Caminante, no hay camino, se hace camino al andar.Al andar se hace camino y al volver la vista atrás se ve la senda que nunca se ha de volver de pisar. Caminante, no hay camino sino estelas en la mar.

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Section: T Rauschermentioning

confidence: 99%

The Path to Improved Reaction Rates for Astrophysics

Rauscher

2011

Int. J. Mod. Phys. E

144

337

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“…and to use averaged quantities C and S which are assumed as being constant [43] or energy-dependent [41,42,44]. Again, the expression can be extended to include sums over thermally populated target states µ.…”

Section: B Relevant Reaction Theorymentioning

confidence: 99%

Large-scale prediction of the parity distribution in the nuclear level density and application to astrophysical reaction rates

et al. 2007

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A generalized method to calculate the excitation-energy dependent parity ratio in the nuclear level density is presented, using the assumption of Poisson distributed independent quasi particles combined with BCS occupation numbers. It is found that it is crucial to employ a sufficiently large model space to allow excitations both from low-lying shells and to higher shells beyond a single major shell. Parity ratios are only found to equilibrate above at least 5-10 MeV of excitation energy. Furthermore, an overshooting effect close to major shells is found where the parity opposite to the ground state parity may dominate across a range of several MeV before the parity ratio finally equilibrates. The method is suited for large-scale calculations as needed, for example, in astrophysical applications. Parity distributions were computed for all nuclei from the proton dripline to the neutron dripline and from Ne up to Bi. These results were then used to recalculate astrophysical reaction rates in a Hauser-Feshbach statistical model. Although certain transitions can be considerably enhanced or suppressed, the impact on astrophysically relevant reactions remains limited, mainly due to the thermal population of target states in stellar reaction rates.

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“…Nuclear structure models cannot predict these states with sufficient accuracy and predicted DC cross sections differ by several orders of magnitude [22]. Furthermore, most DC predictions far off stability have utilized only constant spectroscopic factors so far [23], only few have employed energy-dependent ones [24,25,26]. To circumvent the problem of the exact prediction of final states it has been suggested [24,25,23] to employ averaged properties, i.e.…”

Section: Low-energy Direct Reactionsmentioning

confidence: 99%