Measurement of the<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mmultiscripts><mml:mi>Fe</mml:mi><mml:mprescripts /><mml:none /><mml:mn>60</mml:mn></mml:mmultiscripts><mml:mo stretchy="false">(</mml:mo><mml:mi>n</mml:mi><mml:mo>,</mml:mo><mml:mi>γ</mml:mi><mml:msup><mml:mo stretchy="false">)</mml:mo><mml:mn>61</mml:mn></mml:msup><mml:mi>Fe</mml:mi></mml:math>Cross Section at Stellar Temperatures

Uberseder, E.; Reifarth, R.; Schumann, D.; Dillmann, I.; Domingo‐Pardo, C.; Görres, J.; Heil, M.; Käppeler, F.; Marganiec, J.; Neuhausen, Jörg; Pignatari, M.; Voß, F.; Walter, S.; Wiescher, M.

doi:10.1103/physrevlett.102.151101

Cited by 60 publications

(52 citation statements)

References 32 publications

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“…II.A.4). Illustrative examples in this respect are the successful measurements of the MACS of 60 Fe (Uberseder et al, 2009) and 147 Pm . In the first case, the sample (Schumann et al, 2010) consisted of 1.4 × 10 16 atoms or 1.4 µg and the activation was complicated by the 6 min half life of the 61 Fe, which required 47 repeated irradiations, and by the small capture cross section of 5.7 mb.…”

Section: Activationsmentioning

confidence: 99%

“…In the first case, the sample (Schumann et al, 2010) consisted of 1.4 × 10 16 atoms or 1.4 µg and the activation was complicated by the 6 min half life of the 61 Fe, which required 47 repeated irradiations, and by the small capture cross section of 5.7 mb. Note that the number of atoms and the cross section result reduced by a factor 1.75 compared to the original paper (Uberseder et al, 2009) because of a new precise half-life determination for 60 Fe (Rugel et al, 2009). The second experiment was performed with an even smaller sample of only 28 ng or 1.1 × 10 14 atoms in order to keep the 147 Pm activity (t 1/2 = 2.6 yr) at a reasonable value.…”

Section: Activationsmentioning

confidence: 99%

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Thesprocess: Nuclear physics, stellar models, and observations

et al. 2011

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Nucleosynthesis in the s process takes place in the He burning layers of low mass AGB stars and during the He and C burning phases of massive stars. The s process contributes about half of the element abundances between Cu and Bi in solar system material. Depending on stellar mass and metallicity the resulting s-abundance patterns exhibit characteristic features, which provide comprehensive information for our understanding of the stellar life cycle and for the chemical evolution of galaxies. The rapidly growing body of detailed abundance observations, in particular for AGB and post-AGB stars, for objects in binary systems, and for the very faint metal-poor population represents exciting challenges and constraints for stellar model calculations. Based on updated and improved nuclear physics data for the s-process reaction network, current models are aiming at ab initio solution for the stellar physics related to convection and mixing processes. Progress in the intimately related areas of observations, nuclear and atomic physics, and stellar modeling is reviewed and the corresponding interplay is illustrated by the general abundance patterns of the elements beyond iron and by the effect of sensitive branching points along the sprocess path. The strong variations of the s-process efficiency with metallicity bear also interesting consequences for Galactic chemical evolution.

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Section: Activationsmentioning

confidence: 99%

Section: Activationsmentioning

confidence: 99%

Thesprocess: Nuclear physics, stellar models, and observations

et al. 2011

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“…Material was extracted from the beam stop and iron was chemically separated. The material of this present work was originally used as a target in a cross section measurement of 60 Fe(n,γ) 61 Fe at stellar energies [15]. The 60 Fe from the target was later recovered and 60 Co was chemically removed.…”

Section: Sample Materialsmentioning

confidence: 99%

Activity measurement of Fe60 through the decay of Co60m and confirmation of its half-life

et al. 2017

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The half-life of the neutron-rich nuclide, 60 Fe has been in dispute in recent years. A measurement in 2009 published a value of (2.62 ± 0.04) × 10 6 years, almost twice that of the previously accepted value from 1984 of (1.49 ± 0.27) × 10 6 years. This longer half-life was confirmed in 2015 by a second measurement, resulting in a value of (2.50 ± 0.12) × 10 6 years. All three half-life measurements used the grow-in of the γ-ray lines in 60 Ni from the decay of the ground state of 60 Co (t 1/2 =5.27 years) to determine the activity of a sample with a known number of 60 Fe atoms. In contrast, the work presented here measured the 60 Fe activity directly via the 58.6 keV γ-ray line from the short-lived isomeric state of 60 Co (t 1/2 =10.5 minutes), thus being independent of any possible contamination from long-lived 60g Co. A fraction of the material from the 2015 experiment with a known number of 60 Fe atoms was used for the activity measurement, resulting in a half-life value of (2.72 ± 0.16) × 10 6 years, confirming again the longer half-life. In addition, 60 Fe/ 56 Fe isotopic ratios of samples with two different dilutions of this material were measured with Accelerator Mass Spectrometry (AMS) to determine the number of 60 Fe atoms. Combining this with our activity measurement resulted in a half-life value of (2.69 ± 0.28) × 10 6 years, again agreeing with the longer half-life.

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“…The experimental data are from Refs. [4,[27][28][29][30][31][32]. Macklin et al [29] measured the capture cross sections of 56,57 Fe from 11 to 60 keV.…”

Section: B the Neutron Capture Cross Sectionsmentioning

confidence: 99%

“…In the weak region in massive stars, this process is termed as weak sr-process [3]. For example, a significant amount of 60 Fe can be produced during the high neutron flux in shell carbon burning phase of s-process [4]. This is the result of branching at 59 Fe with the half-life of 44.495 days.…”

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confidence: 99%

Microscopic folding model analysis of the radiative(n,γ)reactions near theZ=28shell closure and the weaksprocess

2016

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Microscopic folding model analysis of the radiative (n, γ) reactions near the Z = 28shell-closure and the weak s-process Saumi Dutta, * G. Gangopadhyay, † and Abhijit Bhattacharyya ‡The radiative thermal neutron capture cross sections over the range of thermal energies from 1 keV to 1 MeV are studied in statistical Hauser-Feshbach formalism. The optical model potential is constructed by folding the density dependent M3Y nucleon-nucleon interaction with radial matter densities of target nuclei obtained from relativistic-mean-field (RMF) theory. The standard nuclear reaction code TALYS1.8 is used for calculation of cross sections. The nuclei studied in the present work reside near the Z = 28 proton shell closure and are of astrophysical interests taking part in p-, s-, and r-process of nucleosynthesis. The Maxwellian-averaged cross-section (MACS) values for energies important for astrophysical applications are presented.

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Measurement of theFe60(n,γ)61FeCross Section at Stellar Temperatures

Cited by 60 publications

References 32 publications

Thesprocess: Nuclear physics, stellar models, and observations

Thesprocess: Nuclear physics, stellar models, and observations

Activity measurement of Fe60 through the decay of Co60m and confirmation of its half-life

Microscopic folding model analysis of the radiative(n,γ)reactions near theZ=28shell closure and the weaksprocess

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