<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mi>β</mml:mi></mml:math>-decay study of neutron-rich bromine and krypton isotopes

Miernik, K.; Rykaczewski, K. P.; Grzywacz, R.; Gross, C. J.; Stracener, D. W.; Batchelder, J. C.; Brewer, N. T.; Cartegni, L.; Fijałkowska, A.; Hamilton, J. H.; Hwang, J. K.; Ilyushkin, S.; Jost, C.; Karny, M.; Korgul, A.; Królas, W.; Liu, S. H.; Madurga, M.; Mazzocchi, C.; Mendez, A. J.; Miller, D.; Padgett, S.; Paulauskas, S. V.; Ramayya, A. V.; Surman, Rebecca; Winger, J. A.; Wolińska-Cichocka, M.; Zganjar, E. F.

doi:10.1103/physrevc.88.014309

Cited by 16 publications

(13 citation statements)

References 43 publications

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“…Although much of the work at the LeRIBSS facility has concentrated on neutron-rich nuclei near -but not on -the r-process path, other results are mentioned here as many of the nuclei measured may provide structure information for r-process post-processing. Using this facility, spectroscopy measurements have been made of 93 Br and 93,94 Kr [282]. The literature values of the decay rates and branching ratios were in good agreement with the measurements.…”

Section: Other Facilitiessupporting

confidence: 65%

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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Section: Other Facilitiessupporting

confidence: 65%

Current Status of r-Process Nucleosynthesis

Kajino,

Aoki,

Balantekin

et al. 2019

Preprint

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“…Recently nuclear masses of interest for the r-process have been measured with Penning traps at the ISOLDE facility at CERN [92], JYFLTRAP at Jyväskylä [93,94], and the CPT at CARIBU [95,96]; via time-of-flight (TOF) at the NSCL [97]; and with the Fragment Separator (FRS) [98] and via Isochronous Mass Spectrometry (IMS) at GSI [99]. New β-decay halflives that impact weak and main r-process simulations have been measured at RIKEN [100,101,102], the NSCL [103,104,105], HRIBF [106,107,108], GSI [109,110,111,112] and CERN/ISOLDE [113]. Neutron capture rates are inaccessible to direct measurements, however innovative indirect techniques are under development and show considerable promise [114,115,116].…”

Section: Introductionmentioning

confidence: 99%

The impact of individual nuclear properties on r-process nucleosynthesis

Mumpower¹,

Surman²,

McLaughlin³

et al. 2016

Progress in Particle and Nuclear Physics

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398

246

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The astrophysical rapid neutron capture process or 'r process' of nucleosynthesis is believed to be responsible for the production of approximately half the heavy element abundances found in nature. This multifaceted problem remains one of the greatest open challenges in all of physics. Knowledge of nuclear physics properties such as masses, β-decay and neutron capture rates, as well as β-delayed neutron emission probabilities are critical inputs that go into calculations of r-process nucleosynthesis. While properties of nuclei near stability have been established, much still remains unknown regarding neutron-rich nuclei far from stability that may participate in the r process. Sensitivity studies gauge the astrophysical response of a change in nuclear physics input(s) which allows for the isolation of the most important nuclear properties that shape the final abundances observed in nature. This review summarizes the extent of recent sensitivity studies and highlights how these studies play a key role in facilitating new insight into the r process. The development of these tools promotes a focused effort for state-of-the-art measurements, motivates construction of new facilities and will ultimately move the community towards addressing the grand challenge of 'How were the elements from iron to uranium made?'. IntroductionOne of the major open questions in all of physics is the identification of the sites responsible for the production of the heaviest elements [1,2]. It has been understood since the 1950s that the solar system abundances of nuclei heavier than iron can be divided roughly in half based on the nucleosynthesis processes that create them. Slow neutron capture process, or s-process, nuclei lie along the middle of the valley of stability, and rapid neutron capture process, or r-process, nuclei are found on the neutron-rich side, with a third process, the p process, responsible for the significantly less abundant nuclei on the proton-rich side of stability [3,4]. Since that time much progress has been made, e.g. [5], and the basic mechanisms of and astrophysical sites for the creation of the s-process [6] and heavy p-process [7,8] nuclei are on a firm footing. The site or sites of the r process still evade definitive determination [9,10,11].The r-process pattern is extracted from the solar system abundances by subtracting the s-process and p-process contributions [12,13]. The residual pattern consists of three main abundance peaks at A ∼ 80, 130, and 195, associated with the N = 50, 82, and 126 closed shells. Building up to the heaviest r-process elements requires on the order of 100 neutrons per seed nucleus. Additional constraints come from meteoritic data, e.g. [14], and observations of r-process elements in old stars in the galactic halo, e.g. [15,16]. This data points to distinct origins for the light A < 120 ('weak') and heavy A > 120 ('main') r-process nuclei. The pattern of main r-process elements is remarkably similar among r-process enhanced halo stars and is a match to the solar residuals. Thi...

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“…The delayed neutron branching ratios P ni are referred from JENDL/FPD-2011 [20] with some corrections reflecting new experimental data [27][28][29][30][31][32][33][34][35], which were obtained after the release of JENDL/FPD-2011.…”

Section: A Fission Product Yieldsmentioning

confidence: 99%

Neutron energy dependence of delayed neutron yields and its assessments

Minato

2018

Journal of Nuclear Science and Technology

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Incident neutron energy dependence of delayed neutron yields of uranium and plutonium isotopes is investigated. A summation calculation of decay and fission yield data is employed, and the energy dependence of the latter part is considered in a phenomenological way. Our calculation systematically reproduces the energy dependence of delayed neutron yields by introducing an energy dependence of the most probable charge and the odd-even effect. The calculated fission yields are assessed by comparison with JENDL/FPY-2011, delayed neutron activities, and decay heats. Although the fission yields in this work are optimized to delayed neutron yields, the calculated decay heats are in good agreement with the experimental data. Comparison of the fission yields calculated in this work and JENDL/FPY-2011 gave an important insight for the evaluation of the next JENDL nuclear data.

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β-decay study of neutron-rich bromine and krypton isotopes

Cited by 16 publications

References 43 publications

Current Status of r-Process Nucleosynthesis

Current Status of r-Process Nucleosynthesis

The impact of individual nuclear properties on r-process nucleosynthesis

Neutron energy dependence of delayed neutron yields and its assessments

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