Nuclear Data Sheets for A = 61

Bhat, M.R.

doi:10.1006/ndsh.1999.0029

Cited by 81 publications

(54 citation statements)

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“…Because of the short half life of 61 Fe (t 1/2 = 5.98 ± 0.06 min [50]), the experiment was divided into 47 repeated irradiations. The irradiations lasted for 15 min, followed by a transfer time of about 60 s from the irradiation position to the counting station, where the activity was measured for 10 min.…”

Section: Experiments On 60 Fe: Technological Frontiersmentioning

confidence: 99%

Stellar neutron capture rates and thesprocess

Käppeler

2012

EPJ Web of Conferences

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Abstract. Neutron reactions are responsible for the formation of the elements heavier than iron. The corresponding scenarios relate to helium burning in Red Giant stars (s process) and to supernova explosions (r and p processes). The s process, which operates in or near the valley of β-stability, has produced about half of the elemental abundances between Fe and Bi. Accurate (n, γ) cross sections are the essential input for s process studies, because they determine the abundances produced by that process. Following a brief summary of the neutron capture processes, the focus will be set on the s process in massive stars, where the role of reliable cross section information is particularly important. Eventually, the intriguing aspects of the origin of 60 Fe will be addressed. Attempts to determine the stellar cross section of that isotope are pushing experimental possibilities to their limits and present a pertinent challenge for future facilities.

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Section: Experiments On 60 Fe: Technological Frontiersmentioning

confidence: 99%

Stellar neutron capture rates and thesprocess

Käppeler

2012

EPJ Web of Conferences

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“…Because of the short half life of 61 Fe (t 1/2 = 5.98 ± 0.06 min [31]), the experiment was divided into 47 runs. The irradiations lasted for 15 min, followed by a transfer time of about 60 s from the irradiation position to the counting station, where the activity was measured for 10 min.…”

Section: Pos(nic X)033mentioning

confidence: 99%

“…The induced activities are characterized by γ-ray lines with known absolute intensities [31,32] and were counted with a pair of HPGe clover detectors, each with a relative efficiency of 120%. By arranging the detectors face to face in very close geometry, absolute peak efficiencies of 56% and 9.5% could be achieved at 100 and 1000 keV, respectively.…”

Section: Pos(nic X)033mentioning

confidence: 99%

Neutron reactions in massive stars and the origin of 60Fe

Käppeler¹

2009

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

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“…The mirror transitions in 61 Zn have energies of 1532, 1141, and 124 keV, respectively [37,38]. A 220 keV transition in 61 Ga finds a natural counterpart in the 89 keV 1/2 − → 3/2 − ground-state transition in 61 Zn [39], but no unique candidate is at hand for the fifth line at 1231 keV. The level schemes of the T z = ±1/2 A = 61 mirror nuclei are shown in Fig.…”

Section: Prompt Particle Decays From Near Spherical States -Mirror Numentioning

confidence: 99%

“…4(a). [39,37,38] and 62 Zn [42] as well as the presumed 2 + and 4 + isobaric analogue states in the odd-odd N = Z nucleus 62 Ga [41]. Energy labels are in keV, tentative transitions and levels are dashed, and the widths of the arrows correspond to the relative intensities of the transitions.…”

Section: Prompt Particle Decays From Near Spherical States -Mirror Numentioning

confidence: 99%