[en] The cross section for $e^{+}{e}^{-<!--\; ???\; -->}$$\to <!--\; ???\; -->$$\mathrm{\eta <!--\; ??\; -->}J/\mathrm{\psi <!--\; ??\; -->}$ between $\sqrt{s}=3.8GeV/c^2$ and 5.3 $GeV/c^2$ is measured via initial state radiation using 980 $f{b}^{-<!--\; ???\; -->1}$ of data on and around the $\mathrm{{\rm Y}<!--\; ??\; -->}(nS)(n=1,2,3,4,5)$ resonances collected with the Belle detector at KEKB. Two resonant structures at the $\mathrm{\psi <!--\; ??\; -->}(4040)$ and $\mathrm{\psi <!--\; ??\; -->}(4160)$ are observed in the $\mathrm{\eta <!--\; ??\; -->}J/\mathrm{\psi <!--\; ??\; -->}$ invariant mass distribution. Fitting the mass spectrum with the coherent sum of two Breit-Wigner functions, one obtains $B$($\mathrm{\psi <!--\; ??\; -->}(4040)\to <!--\; ???\; -->\mathrm{\eta <!--\; ??\; -->}J/\mathrm{\psi <!--\; ??\; -->}$)$\cdot <!--\; ???\; -->{\mathrm{\Gamma <!--\; ??\; -->}}_{e^{+}{e}^{-<!--\; ???\; -->}}^{\mathrm{\psi <!--\; ??\; -->}(4040)}$ = ($4.8\pm <!--\; ??\; -->0.9\pm <!--\; ??\; -->1.4$) eV and $B$($\mathrm{\psi <!--\; ??\; -->}(4160)\to <!--\; ???\; -->\mathrm{\eta <!--\; ??\; -->}J/\mathrm{\psi <!--\; ??\; -->})\cdot <!--\; ???\; -->{\mathrm{\Gamma <!--\; ??\; -->}}_{ee}^{\mathrm{\psi <!--\; ??\; -->}(4160)}$ = ($4.0\pm <!--\; ??\; -->0.8\pm <!--\; ??\; -->1.4$) eV for one solution and $B$($\mathrm{\psi <!--\; ??\; -->}(4040)\to <!--\; ???\; -->\mathrm{\eta <!--\; ??\; -->}J/\mathrm{\psi <!--\; ??\; -->}$)$\cdot <!--\; ???\; -->{\mathrm{\Gamma <!--\; ??\; -->}}_{ee}^{\mathrm{\psi <!--\; ??\; -->}(4040)}$ = ($11.2\pm <!--\; ??\; -->1.3\pm <!--\; ??\; -->1.9$) eV and $B$($\mathrm{\psi <!--\; ??\; -->}(4160)\to <!--\; ???\; -->\mathrm{\eta <!--\; ??\; -->}J/\mathrm{\psi <!--\; ??\; -->}$)$\cdot <!--\; ???\; -->{\mathrm{\Gamma <!--\; ??\; -->}}_{ee}^{\mathrm{\psi <!--\; ??\; -->}(4160)}$ = ($13.8\pm <!--\; ??\; -->1.3\pm <!--\; ??\; -->2.0$) eV for the other solution, where the first errors are statistical and the second are systematic. This is the first measurement of this hadronic transition mode of these two states, and the partial widths to $\mathrm{\eta <!--\; ??\; -->}J/\mathrm{\psi <!--\; ??\; -->}$ are found to be about 1 MeV. There is no evidence for the $Y(4260)$, $Y(4360)$, $\mathrm{\psi <!--\; ??\; -->}(4415)$, or $Y(4660)$ in the $\mathrm{\eta <!--\; ??\; -->}J/\mathrm{\psi <!--\; ??\; -->}$ final state, and upper limits of their production rates in $e^{+}{e}^{-<!--\; ???\; -->}$ annihilation are determined.

[en] Purpose of NPP Fire protection at NPP in Korea is to minimise both probability of occurrence and consequence of fire. To meet this object, operating plants are designed to provide reasonable assurance through defence in depth. Ultimate goal is nuclear safety and Radioactive release to be minimised in the event of a fire. The korea regulatory framework for nuclear plant is based on number for US regulations and supporting guidelines, including but not limited to General Design Criterion. Each plants has their specific licence so, they determine the applicability of a specific regulation to specific plant. In accordance with Korea nuclear regulation Atomic Energy law include fire protection programme to protect structure, system and component important to safety. It also sates about requirement for Fire Hazard Analysis and fire prevention, fire detection system and suppression, building design and etc. After Fukushima accident, regulation is strengthened and many amendments and modification of fire protection system is proceeding to meet the requirement. (author)

[en] The process e⁺e^– → γχ_cJ (J = 1, 2) is studied via initial state radiation using 980 fb^–1 of data at and around the Υ(nS) (n = 1, 2, 3, 4, 5) resonances collected with the Belle detector at the KEKB asymmetric-energy e⁺e^– collider. Here, no significant signal is observed except from ψ(2S) decays. Upper limits on the cross sections between √s = 3.80 and 5.56 GeV are determined at the 90% credibility level, which range from a few pb to a few tens of pb. We also set upper limits on the decay rate of the vector charmonium [ψ(4040), ψ(4160), and ψ(4415)] and charmoniumlike [Y(4260), Y(4360), and Y(4660)] states to γχ_cJ.

[en] Accurate and update assignment of population-related environmental matters onto fine grid cells in oasis cities of arid areas remains challenging. We present the approach based on Suomi National Polar-orbiting Partnership (S-NPP) -Visible Infrared Imaging Radiometer Suite (VIIRS) Day/Night Band (DNB) to reallocate population onto a regular finer surface. The number of potential population to the mercury were reallocated onto 0.1x0.1 km reference grid in Urumqi city cluster of China’s Xinjiang, central Asia. The result of Monte Carlo modelling indicated that the range of 0.5 to 2.4 million people was reliable. The study highlights that the NPP-VIIRS DNB-based multi-layered, dasymetric, spatial method enhances our abilities to remotely estimate the distribution and size of target population at the street-level scale and has the potential to transform control strategies for epidemiology, public policy and other socioeconomic fields. (paper)

[en] The long-lived ⁶⁰Fe (with a half-life of 2.62 Myr) is a crucial diagnostic of active nucleosynthesis in the Milky Way galaxy and in supernovae near the solar system. The neutron-capture reaction ⁵⁹Fe(n,γ)⁶⁰Fe on ⁵⁹Fe (half-life = 44.5 days) is the key reaction for the production of ⁶⁰Fe in massive stars. This reaction cross section has been previously constrained by the Coulomb dissociation experiment, which offered partial constraint on the E1 γ-ray strength function but a negligible constraint on the M1 and E2 components. In this work, for the first time, we use the surrogate ratio method to experimentally determine the ⁵⁹Fe(n,γ)⁶⁰Fe cross sections in which all the components are included. We derived a Maxwellian-averaged cross section of 27.5 ± 3.5 mb at kT = 30 keV and 13.4 ± 1.7 mb at kT = 90 keV, roughly 10%–20% higher than previous estimates. We analyzed the impact of our new reaction rates in nucleosynthesis models of massive stars and found that uncertainties in the production of ⁶⁰Fe from the ⁵⁹Fe(n,γ)⁶⁰Fe rate are at most 25%. We conclude that stellar physics uncertainties now play a major role in the accurate evaluation of the stellar production of ⁶⁰Fe.