Half-lives of heavy nuclei through<i>α</i>tagging

Morales, A. I.

doi:10.1051/epjconf/20146602007

Cited by 5 publications

(5 citation statements)

References 11 publications

(10 reference statements)

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“…It is worth noting the agreement between the values obtained from the β-delayed γ spectra shown here and from the time decay curve of 215 Bi, discussed in Ref. [34]. The analysis of γ -γ coincidences has allowed some γ -decay relationships between new and previously reported transitions to be established.…”

Section: β-Delayed γ Spectrasupporting

confidence: 83%

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β-decay studies of neutron-rich Tl, Pb, and Bi isotopes

Morales¹,

Benzoni²,

Gottardo³

et al. 2014

Phys. Rev. C

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The fragmentation of relativistic uranium projectiles has been exploited at the Gesellschaft für Schwerionenforschung laboratory to investigate the β decay of neutron-rich nuclei just beyond 208 Pb. This paper reports on β-delayed γ decays of [211][212][213] Tl, 215 Pb, and 215-219 Bi de-exciting states in the daughters 211-213 Pb, 215 Bi, and 215-219 Po. The resulting partial level schemes, proposed with the help of systematics and shell-model calculations, are presented. The role of allowed Gamow-Teller and first-forbidden β transitions in this mass region is discussed.

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Section: β-Delayed γ Spectrasupporting

confidence: 83%

“…bring to completion the β decay studies on the fragmentation residues 211-213 Tl and 215-219 Po, for which the half-lives are reported elsewhere [8,34].…”

Section: β-Delayed γ Spectramentioning

confidence: 95%

β-decay studies of neutron-rich Tl, Pb, and Bi isotopes

Morales¹,

Benzoni²,

Gottardo³

et al. 2014

Phys. Rev. C

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“…In the present Letter, we report on the half-lives of [200][201][202] 204 Pt is the lightest N ¼ 126 isotone for which β-decay data are presently available. These results are combined together with other 19 half-lives measured during the "stopped beam" campaign of the rare isotope investigations at GSI (RISING) collaboration [25][26][27][28][29][30] to provide the first systematic comparison with theoretical predictions across the N ¼ 126 shell closure. The location of the nuclei in the Segrè chart is shown in Fig.…”

Section: Infn-laboratori Nazionali DI Legnaro I-35020 Legnaro Italymentioning

confidence: 99%

“…Time-correlated spectra for the N ¼ 126 isotone [25][26][27][28][29][30] with predicted values of FRDM þ QRPA(a) [6], DF3 þ cQRPA (b) [7,8], pn-QRPA (c) [11], and SM (d) [9,37]. [6][7][8][9]11].…”

Section: Infn-laboratori Nazionali DI Legnaro I-35020 Legnaro Italymentioning

confidence: 99%

Half-Life Systematics across theN=126Shell Closure: Role of First-Forbidden Transitions in theβDecay of Heavy Neutron-Rich Nuclei

et al. 2014

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This Letter reports on a systematic study of β-decay half-lives of neutron-rich nuclei around doubly magic 208 Pb. The lifetimes of the 126-neutron shell isotone 204 Pt and the neighboring [200][201][202] Ir, 203 Pt, 204 Au are presented together with other 19 half-lives measured during the "stopped beam" campaign of the rare isotope investigations at GSI collaboration. The results constrain the main nuclear theories used in calculations of r-process nucleosynthesis. Predictions based on a statistical macroscopic description of the first-forbidden β strength reveal significant deviations for most of the nuclei with N < 126. In contrast, theories including a fully microscopic treatment of allowed and first-forbidden transitions reproduce more satisfactorily the trend in the measured half-lives for the nuclei in this region, where the r-process pathway passes through during β decay back to stability. DOI: 10.1103/PhysRevLett.113.022702 PACS numbers: 25.70.Mn, 23.40.-s, 26.30.Hj, 27.80.+w In very hot, neutron-rich stellar environments, the r process of nucleosynthesis is ignited in a series of rapid neutron captures on seed nuclei of the Fe group, thus creating very exotic neutron-rich nuclei that β decay back to stability around the neutron shell closures with N ¼ 50, 82, and 126. In these "waiting-point" regions, matter is accumulated at masses A ∼ 80, 130, and 195, thus creating the so-called first, second, and third r-abundance peaks. These basic features of the r process were established more than half a century ago [1]. However, how the heavy nuclei from Ni to U are synthesized is one of the major unanswered questions of modern physics because of the large uncertainties in the path, time scale, and astrophysical conditions for the rapid neutron capture process to develop [2]. Observational constraints such as the elemental abundances in metal-poor stars or in solar system material help to determine astronomical sites where it might occur [3,4]. Concurrently, β-decay properties of very exotic nuclei near the path, such as β half-lives, are critical in determining the observed abundances [5]. Since many of the r-process progenitors cannot be accessed with present radioactive ion beam facilities, estimates of r-process nucleosynthesis generally rely upon predictions of stateof-the-art nuclear models, based on the properties of nuclei far from stability [6][7][8][9][10][11]. But at extreme values of isospin, theoretical predictions may be biased by microscopic structural effects that modify the shape of the β-strength function, such as nuclear shell quenching or deformation [12,13]. Until now, such theories have only been tested with information on β decay around the first two waiting points

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“…These have been either first-time measurements or improvements on previous measurements. Nuclei that have been measured include 194−196 Re, 199,200 Os, 199−202 Ir, 203,204 Pt, 211−213 Tl, and 219 Bi [268,269,270,271,272,273,274]. Further experiments with the same setup have examined the decay systematics of 211−213 Tl, 215 Pb, and 215−219 Bi including the γ-decay states of the daughter nuclei [275].…”

Section: Gsimentioning

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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Half-lives of heavy nuclei throughαtagging

Abstract: Abstract. Neutron-rich isotopes around lead, beyond N=126, have been studied exploiting the fragmentation of a 238 U beam at 1 GeV/u, at the FRS-RISING setup at GSI. In order to study the half-lives of populated nuclei both α and β correlations have been exploited.

Cited by 5 publications

References 11 publications

β-decay studies of neutron-rich Tl, Pb, and Bi isotopes

β-decay studies of neutron-rich Tl, Pb, and Bi isotopes

Half-Life Systematics across theN=126Shell Closure: Role of First-Forbidden Transitions in theβDecay of Heavy Neutron-Rich Nuclei

Current Status of r-Process Nucleosynthesis

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