Half-life of 178m2Hf and its neutron capture production
References (8)
- et al.
Nucl. Phys.
(1968) - et al.
Nucl. Phys.
(1964) - et al.
Nucl. Phys.
(1968) - et al.
Nucl. Data
(1968)
Cited by (51)
Emergence of an island of extreme nuclear isomerism at high excitation near <sup>208</sup>Pb
2022, Physics Letters, Section B: Nuclear, Elementary Particle and High-Energy PhysicsThe flux weighted cross sections of <sup>179</sup>Hf(γ,γ’)<sup>179m</sup>Hf and <sup>nat</sup>Hf(γ,x)<sup>179m</sup>Hf reactions at 8 MeV and 15 MeV bremsstrahlung end point energies
2021, Applied Radiation and IsotopesCitation Excerpt :There are five stable isotopes of hafnium with mass number varying from 176 to 180. All these isotopes of hafnium have fairly large cross sections for absorption of thermal neutrons, ranging from 13 to 375 b [Alexander and Brinckmann, 1962; Bollinger et al., 1953; Cho et al., 2001; Farina Arboccò et al., 2014; Helmer and Reich, 1973; Krane, 2019; Nguyen et al., 2008; Pomerance, 1952; Vockenhuber et al., 2008], and therefore considered as one of the important elements for the control rods of nuclear reactors [Shikov et al., 2003; Wallenius and Westlén, 2008]. Moreover, hafnium isotopes occur naturally in the form of impurity, around 1–4%, in zirconium ore and therefore difficult to separate it from the zirconium element.
Atlas of Nuclear Isomers
2015, Nuclear Data SheetsNuclear Data Sheets for A = 178
2009, Nuclear Data SheetsProduction of long-lived hafnium isomers in reactor irradiations
2006, High Energy Density Physics<sup>182</sup>Hf, a new isotope for AMS
2004, Nuclear Instruments and Methods in Physics Research, Section B: Beam Interactions with Materials and AtomsCitation Excerpt :Although this uncertainty does not influence relative chronometry, an improvement is desirable for the absolute time scale. We are currently in the process of performing a new half-life measurement using sample material prepared by Helmer and Reich some 40 years ago, which led to the discovery of the 30-year isomer in 178Hf [8,9]. 182Hf is a typical r-process nuclide, but it can also be produced by the so-called “fast” s-process in massive stars [10].
- †
Work performed under the auspices of the US Atomic Energy Commission.