The Effects of the Pickling Process on the Amount of Hydrogen Occluded in Steel Plate for Porcelain Enamel

By direct estimation of the hydrogen content in the enameling steel of the composition C : 0.06, Si : 0.05, Mn: 0.44, P : 0.04, Cu : 0.32% by vacuum heating procedure the authors have confirmed the following facts. (1) The hydrogen absorbed in steel plate of 0.56 mm thick during the pickling with 10% sulphuric acid solution will be removed almost completely if the aftertreatment will be carried out according to the normal schedule. However, with the plate of 6 mm thick a part of hydrogen will remain obstinately even if the after treatments are strictly obeyed to the normal schedule. (2) If the schedule of after. treatment will be changed arbitrary or be simplified then a part of absorbed hydrogen may remain in steel plate so thin as 0.56 mm. (3) A large quantity of hydrogen will remain in steel plate especially when the latter has cavitie3, and a part of hydrogen accumlated in holes can not be removed by the prolonged heating at 70°C

A Spectral Study of the Black Hole Candidate XTE J1752-223 in the High/Soft State with MAXI, Suzaku and Swift

We report on the X-ray spectral analysis of the black hole candidate XTE\ J1752--223 in the 2009--2010 outburst, utilizing data obtained with the MAXI/Gas Slit Camera (GSC), the Swift/XRT, and Suzaku, which work complementarily. As already reported by Nakahira et al. (2010) MAXI monitored the source continuously throughout the entire outburst for about eight months. All the MAXI/GSC energy spectra in the high/soft state lasting for 2 months are well represented by a multi-color disk plus power-law model. The innermost disk temperature changed from $\sim$0.7 keV to $\sim$0.4 keV and the disk flux decreased by an order of magnitude. Nevertheless, the innermost radius is constant at $\sim$41 $D_{3.5}(\cos{\it i})^{-1/2}$ km, where $D_{3.5}$ is the source distance in units of 3.5 kpc and $i$ the inclination. The multi-color disk parameters obtained with the MAXI/GSC are consistent with those with the Swift/XRT and Suzaku. The Suzaku data also suggests a possibility that the disk emission is slightly Comptonized, which could account for broad iron-K features reported previously. Assuming that the obtained innermost radius represents the innermost stable circular orbit for a non-rotating black hole, we estimate the mass of the black hole to be 5.51$\pm$0.28 $M_{\odot}$ $D_{3.5}(\cos{\it i})^{-1/2}$, where the correction for the stress-free inner boundary condition and color hardening factor of 1.7 are taken into account. If the inclination is less than 49$^{\circ}$ as suggested from the radio monitoring of transient jets and the soft-to-hard transition in 2010 April occurred at 1--4% of Eddignton luminosity, the fitting of the Suzaku spectra with a relativistic accretion-disk model derives constraints on the mass and the distance to be 3.1--55 $M_{\odot}$ and 2.3--22 {\rm kpc}, respectively. This confirms that the compact object in XTE J1752--223 is a black hole.Comment: 12 pages including 7 figures and 4 tables, accepted for publication in PAS

KOMI チャート システム オ カツヨウ シタ シュウマツキ カンジャ ノ カンゴ

膀胱腫瘍で終末期にあり,ある程度死に至る過程を理解している男性患者で,出来ることは最期まで自分の力でしたい,家族に迷惑をかけたくない,自分の最期はただ痛みだけをとってほしいという希望をもっている症例に関わった.KOMIチャートシステムを活用し,入院期間中の各期(ADLが自己でまかなえていた時期,徐々にADLが低下した時期,臥床期)に応じた看護を展開した.その結果,同室者を励まし支え合いながら患者らしさを維持でき,望みどおりの最期を迎えさせることができた.この事例を通して,終末期においては患者のニーズを個別的に満たすことや患者背景を把握しそれに伴う苦痛・苦悩に看護師が一体となりアプローチしていくことが重要であることを再認識したWe nursed a patient in terminal stage of bladder cancer using KOMI chart system. He realized his Illness was in terminal stage. His desires were (1) not make his handicapped wife be anxious, (2) want to look after him by himself, (3) not want his families and other persons be worried, We helped him to fulfill his wishes thinking these desires were the source of vital power, As a result, In KOMI reader chart and KOMI chart, he could maintain the role item in recognition throughout his life in spite of the reduction of life\u27s width and behavior. We think we could help him to fulfill his desires

The Quiescent Intracluster Medium in the Core of the Perseus Cluster

Clusters of galaxies are the most massive gravitationally-bound objects in the Universe and are still forming. They are thus important probes of cosmological parameters and a host of astrophysical processes. Knowledge of the dynamics of the pervasive hot gas, which dominates in mass over stars in a cluster, is a crucial missing ingredient. It can enable new insights into mechanical energy injection by the central supermassive black hole and the use of hydrostatic equilibrium for the determination of cluster masses. X-rays from the core of the Perseus cluster are emitted by the 50 million K diffuse hot plasma filling its gravitational potential well. The Active Galactic Nucleus of the central galaxy NGC1275 is pumping jetted energy into the surrounding intracluster medium, creating buoyant bubbles filled with relativistic plasma. These likely induce motions in the intracluster medium and heat the inner gas preventing runaway radiative cooling; a process known as Active Galactic Nucleus Feedback. Here we report on Hitomi X-ray observations of the Perseus cluster core, which reveal a remarkably quiescent atmosphere where the gas has a line-of-sight velocity dispersion of 164+/-10 km/s in a region 30-60 kpc from the central nucleus. A gradient in the line-of-sight velocity of 150+/-70 km/s is found across the 60 kpc image of the cluster core. Turbulent pressure support in the gas is 4% or less of the thermodynamic pressure, with large scale shear at most doubling that estimate. We infer that total cluster masses determined from hydrostatic equilibrium in the central regions need little correction for turbulent pressure.Comment: 31 pages, 11 Figs, published in Nature July