Effects of β-decays of excited-state nuclei on the astrophysical r-process

Famiano, M.; Boyd, R. N.; Kajino, Toshitaka; Otsuki, Kaori; Terasawa, M.; Mathews, Grant J.

doi:10.1088/0954-3899/35/2/025203

Cited by 13 publications

(12 citation statements)

References 40 publications

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“…3, the experimental values for 64 Zn are extracted from Refs. [36] (empty circles), [37] (filled circles) and [38] (empty triangles). The results for 66 Zn are from Skakun et al [38] while those from 67,68 Zn are from Refs.…”

Section: S-factors Of (P γ) Reactionsmentioning

confidence: 99%

Microscopic calculation of proton capture reactions in the mass 60–80 region and its astrophysical implications

Lahiri¹,

Gangopadhyay²

2011

Eur. Phys. J. A

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Microscopic optical potentials obtained by folding the DDM3Y interaction with the densities from Relativistic Mean Field approach have been utilized to evaluate S-factors of low-energy (p, γ) reactions in mass 60-80 region and to compare with experiments. The Lagrangian density FSU Gold has been employed. Astrophysical rates for important proton capture reactions have been calculated to study the behaviour of rapid proton nucleosynthesis for waiting point nuclei with mass less than A = 80.

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Section: S-factors Of (P γ) Reactionsmentioning

confidence: 99%

Microscopic calculation of proton capture reactions in the mass 60–80 region and its astrophysical implications

Lahiri¹,

Gangopadhyay²

2011

Eur. Phys. J. A

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“…The experimental astrophysical S-factors of the 64 Zn(p,γ) 65 Ga, 66 Zn(p,γ) 67 Ga, and 67 Zn(p,γ) 68 Ga reactions (in 10 6 MeV⋅barn) together with theoretical predictions of the new H-F code NON-SMOKER WEB v5.2.1w using different inputs for nuclear properties are compared in Fig. 1 with previous data [12,13]. The results of the standard calculations with the JLM optical potential [14] are given by the thin solid lines while the dashed lines show the quantities calculated with a new low-energy modification of potential [15,16] with subsequent improvement to Lane-consistency [17].…”

Section: Experimental Results and Theoretical Predictionsmentioning

confidence: 99%

Proton capture on 64Zn, 66Zn, and 67Zn between 1 and 3 MeV

Skakun¹

2009

Proceedings of 10th Symposium on Nuclei in the Cosmos — PoS(NIC X)

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Cross sections were determined by the activation technique for the reactions 64 Zn(p,γ) 65 Ga, 66 Zn(p,γ) 67 Ga, and 67 Zn(p,γ) 68 Ga in the center of mass energy range between 1 and 3 MeV using the proton beam of the Van de Graaff accelerator at KIPT, Kharkiv. Thin enriched targets of zinc isotopes on thick tantalum backings were used in the experiment. The radioactivities of 65 Ga, 67 Ga, and 68 Ga were measured by high-resolution γ-ray spectrometry. S-factors and reaction rates were derived from the experimental cross sections and compared with the statistical theory predictions using the new computer code NON-SMOKER WEB. Despite the largely different magnitudes of the cross sections of the first two reactions, theory reproduces the experimental values equally well. Best agreement of the predictions with the experimental data was achieved with a modification of the optical model potential and variation of radiative widths The sensitivity of the results on different theory parameters is studied. This is an important test of the model for proton capture at energies relevant in p-process nucleosynthesis.

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“…In addition to ground state β decay, at the high temperatures of the r-process environment decay can proceed through thermally excited states. In [66] a calculation was made to evaluate the possible effects of the β-decay of nuclei in excited-states on the astrophysical r-process. Single-particle levels were calculated in the FRDM model with quantum numbers determined based upon their proximity to Nilsson model levels.…”

Section: Theoretical β-Decay Ratesmentioning

confidence: 99%

Current Status of r-Process Nucleosynthesis

Kajino,

Aoki,

Balantekin

et al. 2019

Preprint

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The rapid neutron capture process (r-process) is believed to be responsible for about half of the production of the elements heavier than iron and contributes to abundances of some lighter nuclides as well. A universal pattern of r-process element abundances is observed in some metal-poor stars of the Galactic halo. This suggests that a well-regulated combination of astrophysical conditions and nuclear physics conspires to produce such a universal abundance pattern. The search for the astrophysical site for r-process nucleosynthesis has stimulated interdisciplinary research for more than six decades. There is currently much enthusiasm surrounding evidence for r-process nucleosynthesis in binary neutron star mergers in the multiwavelength follow-up observations of kilonova/gravitational-wave GRB170807A/GW170817. Nevertheless, there remain questions as to the contribution over the history of the Galaxy to the current solar-system r-process abundances from other sites such as neutrino-driven winds or magnetohydrodynamical ejection of material from core-collapse supernovae. In this review we highlight some current issues surrounding the nuclear physics input, astronomical observations, galactic chemical evolution, and theoretical simulations of r process astrophysical environments with goal of outlining a path toward resolving the remaining mysteries of the r-process.

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Effects of β-decays of excited-state nuclei on the astrophysical r-process

Cited by 13 publications

References 40 publications

Microscopic calculation of proton capture reactions in the mass 60–80 region and its astrophysical implications

Microscopic calculation of proton capture reactions in the mass 60–80 region and its astrophysical implications

Proton capture on 64Zn, 66Zn, and 67Zn between 1 and 3 MeV

Current Status of r-Process Nucleosynthesis

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