Calculated fission barriers, ground-state masses, and particle separation energies for nuclei with 76 ≤ Z ≤ 100 and 140 ≤ N ≤ 184

Howard, W. M.; Möller, P.

doi:10.1016/0092-640x(80)90005-4

Cited by 158 publications

(152 citation statements)

References 25 publications

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“…3.3). Similar deviations are obtained within the macroscopicmicroscopic approach with the Finite-Range Liquid Drop Model (FRLDM) [62], in particular for primary barriers [61] and those predicted by the HFB-14 [54], FRLDM [62], ETFSI [63], MS99 [64] and HM80 [65] global models for 88 ≤ Z ≤ 96.…”

Section: Fission Pathsupporting

confidence: 71%

The fundamental role of fission during r-process nucleosynthesis in neutron star mergers

Goriely

2015

Eur. Phys. J. A

110

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Abstract. The rapid neutron-capture process, or r-process, is known to be of fundamental importance for explaining the origin of approximately half of the A > 60 stable nuclei observed in nature. Despite important efforts, the astrophysical site of the r-process remains unidentified. Here we study r-process nucleosynthesis in a material that is dynamically ejected by tidal and pressure forces during the merging of binary neutron stars. r-process nucleosynthesis during the decompression is known to be largely insensitive to the detailed astrophysical conditions because of efficient fission recycling, producing a composition that closely follows the solar r-abundance distribution for nuclei with mass numbers A > 140. Due to the important role played by fission in such a scenario, the impact of fission is carefully analyzed. We consider different state-of-the-art global models for the determination of the fission paths, nuclear level densities at the fission saddle points and fission fragment distributions. Based on such models, the sensitivity of the calculated r-process abundance distribution is studied. The fission path is found to strongly affect the region of heavy nuclei responsible for the fission recycling, while the fission fragment distribution of nuclei along the A 278 isobars defines the abundance pattern of nuclei produced in the 110 A 170 region. The late capture of prompt fission neutrons is also shown to affect the abundance distribution, and in particular the shape of the third r-process peak around A 195.

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Section: Fission Pathsupporting

confidence: 71%

The fundamental role of fission during r-process nucleosynthesis in neutron star mergers

Goriely

2015

Eur. Phys. J. A

110

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“…The heights of both barriers f were predicted in the calculations of Howard & Möller (1980) (HM) and Mamdouh et al (2001). However, the TF model predicts only one of the fission barriers.…”

Section: Neutron-induced Fission Rates For a Variety Of Mass Modelsmentioning

confidence: 98%

“…Early r-process calculations (Thielemann et al 1983), which included fission, made use of the mass predictions by Hilf et al (1976) and the fission barriers of a macroscopic-microscopic model by Howard & Möller (1980). For many years different authors used the fission barriers from Howard & Möller (1980), as they were the only complete set of barriers available.…”

Section: Neutron-induced Fission Rates For a Variety Of Mass Modelsmentioning

confidence: 99%

“…For many years different authors used the fission barriers from Howard & Möller (1980), as they were the only complete set of barriers available. More recently, renewed interest (and increased computing power) spurred a number of new calculations of large sets of barrier predictions within various models, resulting on "average" in higher values of fission barriers than predicted by Howard & Möller (1980).…”

Section: Neutron-induced Fission Rates For a Variety Of Mass Modelsmentioning

confidence: 99%

“…For the rates shown here we chose to use the difference in height of the first and second barrier of HM to predict the lower barrier for the TF approach. In this manner, the new fission rate calculations were extended to the region above charge Z = 100, whereas Howard & Möller (1980) presented results only for Z ≤ 100. This allows us to perform r-process calculations in extremely neutron-rich environments as well as to study superheavy element production in rapid neutron capture nucleosynthesis processes.…”

Section: Neutron-induced Fission Rates For a Variety Of Mass Modelsmentioning

confidence: 99%

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Neutron-induced astrophysical reaction rates for translead nuclei

Panov

Korneev

Rauscher

et al. 2010

A&A

116

107

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Neutron-induced reaction rates, including fission and neutron capture, are calculated in the temperature range 10 8 ≤ T (K) ≤ 10 10 within the framework of the statistical model for targets with the atomic number 84 ≤ Z ≤ 118 (from Po to Uuo) from the neutron to the proton drip-line. Four sets of rates have been calculated, utilizing -where possible -consistent nuclear data for neutron separation energies and fission barriers from Thomas-Fermi (TF), Extended Thomas-Fermi plus Strutinsky Integral (ETFSI), Finite-Range Droplet Model (FRDM) and Hartree-Fock-Bogolyubov (HFB) predictions. Tables of calculated values as well as analytic seven parameter fits in the standard REACLIB format are supplied. We also discuss the sensitivity of the rates to the input, aiming at a better understanding of the variations introduced by the nuclear input.

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Beta Decay Far from Stability and Its Role in Nuclear Physics and Astrophysics

Klapdor

1985

Fortschr. Phys.

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Calculated fission barriers, ground-state masses, and particle separation energies for nuclei with 76 ≤ Z ≤ 100 and 140 ≤ N ≤ 184

Cited by 158 publications

References 25 publications

The fundamental role of fission during r-process nucleosynthesis in neutron star mergers

The fundamental role of fission during r-process nucleosynthesis in neutron star mergers

Neutron-induced astrophysical reaction rates for translead nuclei

Beta Decay Far from Stability and Its Role in Nuclear Physics and Astrophysics

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