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In mathematics education, understanding the concepts of given domains in terms of conceptual and procedural knowledge is essential. We have developed a framework for case study of children studying mathematical logic and related concepts using the automated theorem proving software Theorema. Theorema allows the user to organize mathematical knowledge as hierarchies of interdependent theories. Here, we present a framework for exploring the different inference processes of children studying mathematical logic using the Theorema software’s automated proof generator.

A 63-year-old man with epigastralgia was referred to our hospital and diagnosed with simultaneous multiple gastric cancers. One lesion was type 2 advanced and the other was type 0- II c early gastric cancer. CT examination revealed 4 regional lymph node metastases. Neoadjuvant chemotherapy(NAC)with docetaxel/CDDP/S-1was administered. After 2 courses of NAC, total gastrectomy with D2(-No. 10), lymphadenectomy was performed. The pathological response to NAC was judged to be Grade 3 for advanced gastric cancer and Grade 0 for early gastric cancer. The patient is alive with no evidence of disease during the 10 months after the operation.

International audience; We have resolved for the first time the radial and vertical structures of the almost edge-on envelope/disc system of the low-mass Class 0 protostar L1527. For that, we have used Atacama Large Millimetre/submillimetre Array (ALMA) observations with a spatial resolution of 0.25 × 0.13 arcsec2 and 0.37 × 0.23 arcsec2 at 0.8 and 1.2 mm, respectively. The L1527 dust continuum emission has a deconvolved size of 78 × 21 au2, and shows a flared disc-like structure. A thin infalling-rotating envelope is seen in the CCH emission outward of about 150 au, and its thickness is increased by a factor of 2 inward of it. This radius lies between the centrifugal radius (200 au) and the centrifugal barrier of the infalling-rotating envelope (100 au). The gas stagnates in front of the centrifugal barrier and moves towards vertical directions. SO emission is concentrated around and inside the centrifugal barrier. The rotation speed of the SO emitting gas is found to be decelerated around the centrifugal barrier. A part of the angular momentum could be extracted by the gas that moves away from the mid-plane around the centrifugal barrier. If this is the case, the centrifugal barrier would be related to the launching mechanism of low-velocity outflows, such as disc winds.

The Class 0 protostar, L483, has been observed in various molecular lines in the 1.2 mm band at a sub-arcsecond resolution with ALMA. An infalling-rotating envelope is traced by the CS line, while a very compact component with a broad velocity width is observed for the CS, SO, HNCO, NH$_2$CHO, and HCOOCH$_3$ lines. Although this source is regarded as the warm carbon-chain chemistry (WCCC) candidate source at a 1000 au scale, complex organic molecules characteristic of hot corinos such as NH$_2$CHO and HCOOCH$_3$ are detected in the vicinity of the protostar. Thus, both hot corino chemistry and WCCC are seen in L483. Although such a mixed chemical character source has been recognized as an intermediate source in previous single-dish observations, we here report the first spatially-resolved detection. A kinematic structure of the infalling-rotating envelope is roughly explained by a simple ballistic model with the protostellar mass of 0.1--0.2 $M_\odot$ and the radius of the centrifugal barrier (a half of the centrifugal radius) of 30--200 au, assuming the inclination angle of 80\degr\ (0\degr\ for a face-on). The broad line emission observed in the above molecules most likely comes from the disk component inside the centrifugal barrier. Thus, a drastic chemical change is seen around the centrifugal barrier., Comment: accepted to ApJ

The global water cycle in the Earth is one of the most important issues in geodynamics, because water can affect the physical and rheological properties of the mantle. However, it is still a matter of debate whether water can be transported into the lower mantle and core. Here we report a new reaction between aluminous perovskite and water to form alumina-depleted perovskite and hydrous δ-phase AlOOH–MgSiO2(OH)2 along the mantle geotherm in the lower mantle. Chemical analysis of the coexisting phases showed that the perovskite and post-perovskite phases were depleted in Al2O3, whereas hydrous δ-phase contains at least 44 mol% of MgSiO2(OH)2 component at 68 GPa and 2010 K, and 23 mol% of this component at 128 GPa and 2190 K. The present experiments revealed that hydrous δ-phase AlOOH–MgSiO2(OH)2 can coexist with alumina-depleted MgSiO3 perovskite or post-perovskite under the lower mantle conditions along the slab geotherm. Thus this hydrous phase in the slabs can transport water into the base of the lower mantle.

Valence, spin states, and crystallographic sites of Fe in (Mg,Fe)SiO 3 perovskite were investigated using energy-domain 57 Fe-synchrotron Mossbauer spectroscopy and powder X-ray diffraction up to 86 GPa. The volumes of Fe 3+ -bearing perovskite in this study are slightly smaller than those of Mg end-member perovskite. Our Mossbauer data suggest that Fe 3+ prefers A sites coupled with Mg vacancies, which is consistent with previous data at ambient conditions. Fe 3+ in the A site remains in a high-spin state up to 86 GPa, and some fraction of the A site is occupied by Fe 2+ at pressures above 30 GPa. Fe 2+ in the A sites is also in a high-spin state up to 86 GPa. The coupled substitution from Mg 2+ to a high-spin state of Fe 3+ and Mg 2+ vacancy would make the volume of perovskite smaller than that of Mg end-member perovskite. If the lower mantle is saturated in silica, perovskite containing high-spin Fe 3+ in A site has a higher density. Such silica oversaturated regions could sink by the density difference.

昨今、化粧に対する関心をもつ女性が幅広い年代で増加している。本研究では女子学生の化粧行動と意識の関連についてアンケート調査を行い考察した。また、印象評価は化粧イメージ画像を作成しSD法を用いて印象評定を行い、因子分析及びクラスター分析により化粧の種類と印象の関係を検討した。その結果、女子学生の化粧導入時期の若年化に加えて化粧意識の高さや化粧行動も積極的であることと、顔の悩み部位は「鼻」が多いにも関わらず、所持している化粧アイテムは「マスカラ」が最も多く、メイク方法では「目」を重視していることが明らかになった。また、4種類3段階の化粧による印象評価では、第1因子の化粧の度合い(薄い-厚い)、第2因子の化粧の色味(冷たい一暖かい)、第3因子の化粧の印象(くどい-あっさり)の3つの因子が抽出された。この因子の組み合わせとクラスター分析によるグループ分けを合わせると、女子学生に好まれる化粧は、「素顔に近すぎず」、かといって派手ではなく、種類としては「女性らしく可愛いナチュラルなイメージ」の化粧の第1段階であった。印象評定の刺激には使用しなかったが同じ種類の第2段階が次いで好まれた。そして前述のように化粧における重要なポイントは目であるものの、派手で過剰なものは敬遠されやすいことが明らかとなった。これらから、現代では様々なメディアによって個性的な化粧のあり方が認められているように見えながら、化粧行動と意識においては思ったほどの多様性は好まれず、概ね同じような印象のものが選ばれていることも明らかとなった。

The equation of state of Fe3S was investigated up to 200 GPa at room temperature using a diamond anvil cell. Fe3S adopts a tetragonal structure up to 200 GPa and no phase transition was observed. The fourth-order Birch–Murnaghan equation of state (EOS) was fitted to present compression data at room temperature. The elastic parameters, such as bulk modulus (K0), its pressure derivative ( K 0 ′ ), and K 0 ″ ( d K ′ / d P ) were determined to be 122.4(50) GPa, 5.36(48), and −0.066(30) GPa−1, respectively by fixing the zero pressure volume, V0, to be 377 A3. Based on fourth-order Birch–Murnaghan EOS of Fe3S, the maximum amount of S in the inner core was estimated to be 11.4(14) at.% based on the density deficit of the inner core.

Pure iron and Fe0.9Ni0.1 alloy were compressed to a pressure of 279 GPa and 272 GPa, respectively. The compression data sets were fitted using the third order Birch–Murnaghan equation of state based on six different pressure scales. Our result shows the nickel increase the density and the c/a ratio, decrease the bulk modulus. The high temperature data obtained the thermal equation of state parameters. At high temperature, although the nickel effect on density slightly decrease due to the a little larger thermal expansion, the bulk modulus difference increase to 7.3–7.8% at 329 GPa and 5000 K. Nickel effects on elasticity might be important at multimegabar pressure and especially high temperature such as the inner core condition. The core density deficit was estimated to be 3.4(1)–5.1(1)% for pure iron and 4.7(1)–6.5(2)% for Fe0.9Ni0.1 alloy if the temperature at the inner core boundary is 5000 K.

We measured the sound velocity of Fe3S at room temperature up to 85 GPa employing inelastic X-ray scattering to better constrain the constitution of the inner core. The density of Fe3S was also determined by X-ray diffraction under the same conditions. The relation of the P-wave velocity ( v P) and density (ρ) of Fe3S follows Birch’s law, v P(m/s) = 1.14(5) × ρ(kg/m3) − 2580(410). Based on Birch’s law determined here for Fe3S and that for ɛ-Fe reported previously, we found that sulfur decreases both density and compressional velocity of hcp-Fe at the core pressure and 300 K.

We investigated the factors determining the distribution and dynamics of tree species in a warm–temperate mature mixed forest of evergreen coniferous and broad-leaved tree species in a steep mountainous area for 13 years in southwest Japan, with particular focus on instability of the ground surface. Among various site conditions, landform unit was the principal factor determining the distribution of tree species, while moisture regime was the second-most important factor within the upper area. The amount of movement of sediment and litter on the ground surface in the lower area was much higher than movement within the upper area, indicating that the lower area was unstable due to mass movement caused by erosion. The effects of instability of the ground surface on mortality and recruitment varied across the dominant tree species. Symplocos prunifolia (SYMPLOCACEAE), which was distributed in the upper area, and Machilus japonica, which was distributed in the lower area, exhibited lower mortality and higher recruitment in the areas where they were mainly distributed. These results suggest that topographic niche differentiation caused habitat segregation for some species. However, for most species, such relationships were not consistently observed, and growth rates did not significantly differ between the upper and lower areas. This study, by using long-term data, demonstrates that variation in sensitivity to stability due to topography contributes to local species richness and co-existence.

The usefulness of magnifying endoscopy with narrow-band imaging (ME-NBI) for the diagnosis of early gastric cancer is well known, however, there are no evaluation criteria. The aim of this study was to devise and evaluate a novel diagnostic algorithm for ME-NBI in depressed early gastric cancer. Between August, 2007 and May, 2011, 90 patients with a total of 110 depressed gastric lesions were enrolled in the study. A diagnostic algorithm was devised based on ME-NBI microvascular findings: microvascular irregularity and abnormal microvascular patterns (fine network, corkscrew and unclassified patterns). The diagnostic efficiency of the algorithm for gastric cancer and histological grade was assessed by measuring its mean sensitivity, specificity, positive predictive value (PPV), negative predictive value (NPV), and accuracy. Furthermore, inter- and intra-observer variation were measured. In the differential diagnosis of gastric cancer from non-cancerous lesions, the mean sensitivity, specificity, PPV, NPV, and accuracy of the diagnostic algorithm were 86.7, 48.0, 94.4, 26.7, and 83.2%, respectively. Furthermore, in the differential diagnosis of undifferentiated adenocarcinoma from differentiated adenocarcinoma, the mean sensitivity, specificity, PPV, NPV, and accuracy of the diagnostic algorithm were 61.6, 86.3, 69.0, 84.8, and 79.1%, respectively. For the ME-NBI final diagnosis using this algorithm, the mean κ values for inter- and intra-observer agreement were 0.50 and 0.77, respectively. In conclusion, the diagnostic algorithm based on ME-NBI microvascular findings was convenient and had high diagnostic accuracy, reliability and reproducibility in the differential diagnosis of depressed gastric lesions.

[1] We determined the compressional velocity of hcp-Fe using high-resolution inelastic X-ray scattering combined with in situ X-ray powder diffraction: Our measurements extend up to 174 GPa at room temperature, to 88 GPa at 700 K, and to 61.5 GPa at 1000 K. Our data, including those obtained at high temperature, are well described by a linear relation to density, extending the range of verification of Birch's law and suggesting only small temperature dependence up to 1000 K. This result, once compared to the preliminary reference Earth model seismologically based model, indicates that there is either a strong temperature effect on Birch's law above 1000 K or the composition of the core is rather different than expected, containing, e.g., heavy impurities. Noting that both recent theoretical calculations and shock wave velocity measurements are consistent with modification of Birch's law at high temperature, we favor the former explanation.

Computed tomography (CT) for light materials such as soft biological tissues was performed using a monochromatic X-ray beam provided by a parametric X-ray radiation (PXR) source at the Laboratory for Electron Beam Research and Application (LEBRA) of Nihon University. Using a high-efficiency flat panel detector (FPD), each projection image for CT was taken with exposure times of 5 or 10 s, and 60–360 projection images in each run were obtained with total measurement time of 5 min to 1 h. CT images were obtained from the projection images using the conventional calculation method. The typical tomograms obtained had sharp outlines, which are likely attributable to the propagation-based phase contrast.

Albitic feldspar in shocked ordinary chondrites (Yamato 791384 L6 and Yamato 75100 H6) and albite recovered from static high-pressure and high-temperature synthetic experiments ( Kubo et al., 2010 ) were investigated with a transmission electron microscope (TEM) subsequent to a conventional micro-Raman spectroscopy analysis to clarify albite dissociation reaction under high-pressure and high-temperature condition. When jadeite forms from albite, SiO 2 phase as a residual phase of albite dissociation reaction should accompany jadeite from the stoichiometry. However, albitic feldspar in and adjacent to shock-melt veins of the shocked chondrites dissociates into jadeite+residual amorphous (or poorly-crystallized) material having varied chemical compositions between jadeite and SiO 2 phase. TEM observations of albitic feldspar in the shocked chondrites and albite recovered from the static high-pressure and high-temperature synthetic experiments show that jadeite crystallization is initiated by grain refinement of albite (or albitic feldspar). Nucleation occurs along grain-boundaries or at triple-junctions of the fine-grained albite crystal assemblage. Jadeite crystal starts to grow from the nucleus through grain-boundary diffusion. Considering pressure condition recorded in the shock-melt veins of the shocked chondrites, stishovite is the most likely as a residual SiO 2 phase accompanying jadeite. High-pressure and high-temperature condition induced by a dynamic event is very short. Stishovite would be hardy formed through a dynamic event due to sluggish nucleation rate of stishovite compared with that of jadeite, thus leading to induce heterogeneous and incomplete albite dissociation reaction; albite dissociates into jadeite+residual amorphous material.

We present a case of classical Hodgkin's lymphoma (HL) co-occurring with histological features of Castleman's disease (CD). A 25-year-old man presented with left supraclavicular and axillary lymph node swelling and mediastinal mass. Using an initial biopsy specimen from left axillary lymph node, a tentative diagnosis of multicentric CD of plasma cell type was made. The serum level of interleukin-6 (IL-6) was elevated. The patient was treated with immunosuppressive therapy containing tocilizumab (TCZ). Shrinkage of mediastinal mass and axillary lymph nodes was seen; however, swelling of his left axillary lymph nodes reemerged, even after therapy with TCZ. A second left axillary lymph node biopsy was performed and a diagnosis of nodular sclerosis of classical HL without histologic features of CD was made. The initial biopsy specimen was re-examined, and scattered CD30+ Hodgkin/Reed-Sternberg cells were found in the interfollicular area. Interestingly, Hodgkin/Reed-Sternberg cells and surrounding reactive cells in both lymph nodes were stained with anti-IL-6 antibody. We emphasize that biopsy specimens with HL involvement may also have histologic features reminiscent of those seen in CD. To our knowledge, this is the first report to provide a detailed description of this pathology, including a survey of IL-6 and clinical course upon treatment with TCZ.

A field experiment to clarify the characteristics of temperature distribution near an asphalt road was carried out at the Meteorological Instruments Center in Tsukuba, Japan. Fifteen thermometers equipped with artificially ventilated radiation shields were installed within a distance of 10 m from the road, and the results showed that the road’s presence caused a significant positive bias at a height of 0.5 m on its leeward side. Thermometers nearer the road showed larger positive biases. The biases tended to be larger in summer than in winter, with greater temporal variations in cases of lower wind speed. At a height of 1.5 m above the ground, small positive biases were seen near the road. At a height of 2.5 m, smaller negative biases were seen with distance from the road. Biases showed diurnal variations with slightly negative values at around daybreak and positive values from late morning to midnight as well as an evening peak in summer. In winter, positive biases were observed throughout the night, while negative biases were seen during the day.

This article is a study record of Mathematics education lessons observed in the teacher training colleges（Instituto de Formação de Professores： IFP） and primary schools of Mozambique. Even though group works（workshop type lesson） were introduced in Mathematics lessons of the IFPs, it didn't work appropriately for the students to remember the definition and meaning intended by the curriculum or lesson plan due to a lack of blackboard management（how to write on blackboard）, worksheet and guidance on note taking. As well as the IFPs, this issue was crucial in the primary schools. Moreover, management of lesson time was also pointed out by authors as one of the most indispensable problems. In both types of educational institutions, it is urgent to improve teachers' knowledge and higher-ordered-thinking skill of Mathematics before enhancing their teaching skills and methods.

In situ X-ray diffraction experiments in the Fe–Fe 3 S system were performed up to 175 GPa and 3500 K using a laser-heated diamond anvil cell to investigate melting relationships in the system. Partial melting in the Fe–Fe 3 S system was observed based on the disappearance of X-ray diffraction peaks of solid Fe 3 S and texture observation of the recovered samples. The melting relationship of the Fe–Fe 3 S system as a function of pressure is evaluated based on Kraut–Kennedy law. Our results of melting relationships suggest that the temperature at the inner core boundary is between 4700(160) and 4930(330) K if sulfur is the only light element in the Earth's core. Assuming the adiabatic temperature gradient in the outer core, the temperature at the core–mantle boundary is estimated to be in the range of 3600–3770 K. The present temperature profile of the core is consistent with the core–mantle boundary temperature that can explain the core heat flux to maintain the core dynamo and the seismic structure at the base of the lower mantle.

The MgSiO3 post-perovskite phase is the most abundant silicate phase in a super-Earth’s mantle, although it only exists within the Earth’s lowermost mantle. In this study, we established the thermal equation of state (EoS) of the MgSiO3 post-perovskite phase, which were determined by using both laser-heated diamond anvil cell and density-functional theoretical techniques, within a multi-megabar pressure range, corresponding to the conditions of a super-Earth’s mantle. The Keane and AP2 EoS models were adopted for the first time to extract meaningful physical properties. The experimentally determined Grüneisen parameter, which is one of the thermal EoS parameters and its volume dependence were found to be consistent with their theoretically obtained values. This reduced the previously reported discrepancy observed between experiment and theory. Both the experimental and theoretical EoS were also found to be in very good agreement for volumes at pressures and temperatures of up to 300 GPa and 5000 K, respectively. Our newly developed EoS should be applicable to a super-Earth’s mantle, as well as the Earth’s core-mantle boundary region.

Experimental determination of VP of hcp-Fe can show potential candidates for major light elements in Earth’s inner core., Hexagonal close-packed iron (hcp-Fe) is a main component of Earth’s inner core. The difference in density between hcp-Fe and the inner core in the Preliminary Reference Earth Model (PREM) shows a density deficit, which implies an existence of light elements in the core. Sound velocities then provide an important constraint on the amount and kind of light elements in the core. Although seismological observations provide density–sound velocity data of Earth’s core, there are few measurements in controlled laboratory conditions for comparison. We report the compressional sound velocity (VP) of hcp-Fe up to 163 GPa and 3000 K using inelastic x-ray scattering from a laser-heated sample in a diamond anvil cell. We propose a new high-temperature Birch’s law for hcp-Fe, which gives us the VP of pure hcp-Fe up to core conditions. We find that Earth’s inner core has a 4 to 5% smaller density and a 4 to 10% smaller VP than hcp-Fe. Our results demonstrate that components other than Fe in Earth’s core are required to explain Earth’s core density and velocity deficits compared to hcp-Fe. Assuming that the temperature effects on iron alloys are the same as those on hcp-Fe, we narrow down light elements in the inner core in terms of the velocity deficit. Hydrogen is a good candidate; thus, Earth’s core may be a hidden hydrogen reservoir. Silicon and sulfur are also possible candidates and could show good agreement with PREM if we consider the presence of some melt in the inner core, anelasticity, and/or a premelting effect.

The hydrous mineral, δ-AlOOH, is stable up to at least the core-mantle boundary, and therefore has been proposed as a water carrier to the Earth’s deep mantle. If δ-AlOOH is transported down to the core-mantle boundary by a subducting slab or the mantle convection, then the reaction between the iron alloy core and δ-AlOOH is important in the deep water/hydrogen cycle in the Earth. Here we conducted an in situ X-ray diffraction study to determine the behavior of hydrogen between Fe–Ni alloys and δ-AlOOH up to near the core-mantle boundary conditions. The obtained diffraction spectra show that fcc/dhcp Fe–Ni hydride is stable over a wide pressure range of 19–121 GPa at high temperatures. Although the temperature of formation of Fe–Ni hydride tends to increase up to 1950 K with increasing pressure to 121 GPa, this reaction temperature is well below the mantle geotherm. δ-AlOOH was confirmed to coexist stably with perovskite, suggesting that δ-AlOOH can be a major hydrous phase in the lower mantle. Therefore, when δ-AlOOH contacts with the core at the core-mantle boundary, the hydrogen is likely to dissolve into the Earth’s core. Based on the present results, the amount of hydrogen to explain the core density deficit is estimated to be 1.0–2.0 wt.%.

We have determined the density evolution of the sound velocity of dhcp-FeHx (x ≈ 1) up to 70 GPa at room temperature, by inelastic X-ray scattering and by X-ray diffraction. We find that the variation of VP with density is different for the ferromagnetic and nonmagnetic dhcp-FeHx, and that only nonmagnetic dhcp-FeHx follows Birch's law. Combining our results with Birch's law for iron and assuming an ideal two-component mixing model, we obtain an upper bound of the hydrogen content in the Earth's inner core, 0.23(6) wt.% H, corresponding to FeH0.13(3). The iron alloy with 0.23(6) wt.% H can satisfy the density, and compressional and shear sound velocities of the PREM inner core, assuming that there are no other light elements in the inner core.

In the application of lasers in dentistry, there is a delicate balance between the benefits gained from laser treatment and the heat-related damage arising from laser irradiation. Hence, it is necessary to understand the different processes associated with the irradiation of lasers on dental materials. To obtain insight for the development of a safe and general-purpose laser for dentistry, the present study examines the physical effects associated with the irradiation of a near-infrared free-electron laser (FEL) on the surface of a commonly used silver dental alloy. The irradiation experiments using a 2900-nm FEL confirmed the formation of a pit in the dental alloy. The pit was formed with one macro-pulse of FEL irradiation, therefore, suggesting the possibility of efficient material processing with an FEL. Additionally, there was only a slight increase in the silver alloy temperature (less than 0.9 °C) despite the long duration of FEL irradiation, thus inferring that fixed prostheses in the oral cavity can be processed by FEL without thermal damage to the surrounding tissue. These results indicate that dental hard tissues and dental materials in the oral cavity can be safely and efficiently processed by the irradiation of a laser, which has the high repetition rate of a femtosecond laser pulse with a wavelength around 2900 nm.

This study was conducted to investigate the distribution of rotavirus genotypes in Nara Prefecture, Japan before and after the introduction of rotavirus vaccination in 2011. Since the 2011/2012 season, DS-1-like G1P[8] strains have been detected in Nara Prefecture, accounting for about half of all strains in the 2014/2015 season. During the 2015/2016 season, no DS-1-like G1P[8] strains were detected; G2P[4] was the predominant genotype.

We have observed the J = 2–1 rotational emission line of PN toward the low-mass star forming region L 1157 with the Nobeyama 45 m telescope. The PN line has been detected toward the two shocked regions (B1 and B2) caused by the interaction between the blue lobe of the outflow from the protostar IRAS 20386+6751 and the ambient gas, whereas it has not been detected toward the protostar position. The fractional abundances of PN relative to H2 are evaluated to be (2–6) � 10 � 10 and (3–7) � 10 � 10 toward B1 and B2, respectively. Detection of PN in the B1 and B2 positions indicates that the formation of PN can be triggered by shocks. It seems most likely that PN is formed in the gas phase from PH3 evaporated from grain mantles, as suggested by the existing chemical model.

The pressure–volume equations of state of iron–nickel–silicon alloy Fe0.83Ni0.09Si0.08 (Fe-9.8 wt.% Ni-4.0 wt.% Si) and iron–silicon alloy Fe0.93Si0.07 (Fe-3.4 wt.% Si) have been investigated up to 374 GPa and 252 GPa, respectively. The present compression data covered pressures of the Earth's core. We confirmed that both Fe0.83Ni0.09Si0.08 and Fe0.93Si0.07 alloys remain in the hexagonal close packed structure at all pressures studied. We obtained the density of these alloys at the pressure of the inner core boundary (ICB), 330 GPa at 300 K by fitting the compression data to the third order Birch–Murnaghan equation of state. Using these density values combined with the previous data for hcp-Fe, hcp-Fe0.8Ni0.2, and hcp-Fe0.84Si0.16 alloys and comparing with the density of the PREM inner core, we estimated the Ni and Si contents of the inner core. The Si content of the inner core estimated here is slightly greater than that estimated previously based on the sound velocity measurement of the hcp-Fe–Ni–Si alloy at high pressure.

An in situ synchrotron powder X-ray diffraction study on (Fe 0.89 ,Ni 0.11 ) 3 S was conducted up to 141 GPa and 1590 K. (Fe 0.89 ,Ni 0.11 ) 3 S has a tetragonal structure, which is the same structure as Ni-free Fe 3 S. Fitting a third-order Birch-Murnaghan equation of state to data at ambient temperature yielded a bulk modulus of K 0 = 138.1(7.2) GPa and its pressure derivative K 0 ′ = 4.5(3) with a zero pressure volume V 0 = 375.67(4) A 3 . The density of (Fe 0.89 ,Ni 0.11 ) 3 S under the core-mantle boundary condition is 1.7% greater than that of Fe 3 S. The axial ratio ( c/a ) of (Fe 0.89 ,Ni 0.11 ) 3 S decreases with increasing pressure. The addition of nickel to Fe 3 S leads to a softening of the c -axis. Assuming that the nickel content of the outer core is about 5 at%, we estimated 12.3–20.8 at% sulfur in the outer core for the given 6–10% density deficit between the outer core and pure iron at 136 GPa.

We have conducted a sensitive 3 mm observation toward the shocked region, Lynds 1157 B1, which is an interaction spot between a molecular outflow and its ambient gas. We have successfully detected the CH3CHO, HCOOCH3, and HCOOH lines, as well as the CH2DOH line. The abundances of these molecules relative to CH3OH are found to be lower than those in the low-mass star-forming core, IRAS 16293� 2422. Since these molecules are thought to evaporate from grain mantles, the observational results mean that complex molecules are less abundant in grain mantles residing in the ambient cloud surrounding a prestellar/protostellar core. Instead, efficient formation of the complex organic species and deuterated species should take place in a prestellar/protostellar core. The present result verifies the importance of an unbiased line survey of this source.

The solidus and liquidus temperatures of the Fe75O5S20 alloy are determined up to 157 GPa using a laser-heated diamond anvil cell combined with in situ X-ray diffraction technique. Fe (fcc/hcp), Fe3S2/Fe3S, and FeO B1/B8/rhombohedral phases are stable under subsolidus conditions. First, Fe3S2 or Fe3S phase melts at a temperature close to the eutectic point of the Fe–Fe3S system, suggesting that the alloying effect of 5 at.% oxygen on the eutectic temperature in the Fe–Fe3S system is minor. Then FeO melts at several hundreds of degrees Kelvin higher than the solidus, and Fe is a liquidus phase in this system. The liquidus temperature is 260–670 K lower than the melting temperature of pure Fe because of the alloying effect of S and O on the melting temperature of Fe. Based on our results, the temperatures at the core/mantle boundary (TCMB) and at the boundary of the inner/outer core (TICB) are estimated to be 3600 ± 200

東シナ海のアカアマダイ漁業と資源状態は 1990 年代に大きく変わったことから，生物特性も変化している可能性があり，本種の成長と成熟を再検討した。産卵盛期は 9, 10 月，50% 成熟全長は雌雄それぞれ 253 mm, 302 mm であった。成長式は雌雄それぞれ l(t)=375(1−e−0.317(t+0.420)) と l(t)=520(1−e−0.194(t+0.761)) と推定された。これらの結果は概ね既往の研究と一致したが，東シナ海内でも海域によって成熟個体の出現などが異なった。今後，資源解析に基づく管理方策及び漁場利用の検討が必要である。

Atomic motions and, especially, correlations in atomic motion over angstrom length scales are a sensitive probe of material properties: phonons in single crystals respond to the detailed interactions between atoms, including both short- and long-range forces, and screening thereof, while the atomic dynamics of liquids is intimately connected with nearly all aspects of liquid behavior. Scientific questions associated with measuring dynamics include the detailed nature of phase transitions, correlations of atomic motions with electronic or magnetic properties (superconductivity, ferro-electric behavior, magnetoelastic coupling, etc.), and also very practical issues, such as investigating elasticity. Not surprisingly, both from the point of view of basic science and for applications such as geology, there is strong desire to extend studies of atomic dynamics throughout material phase diagrams, into extreme conditions.

In order to minimize the size of the X-ray source for a U-shaped rotating anticathode X-ray generator, the electron beam is focused over a short distance by a combined-function bending magnet. Simulation predicts that the beam brightness will reach almost 500 kW mm−2 for a 120 keV/75 mA beam., A new type of rotating anticathode X-ray generator, where an electron beam of up to 60 keV irradiates the inner surface of a U-shaped Cu anticathode, has achieved a beam brilliance of 130 kW mm−2 (at 2.3 kW). A higher-flux electron beam is expected from simulation by optimizing the geometry of a combined-function-type magnet instead of the fringing field of the bending magnet. In order to minimize the size of the X-ray source the electron beam has been focused over a short distance by a new combined-function bending magnet, whose geometrical shape was determined by simulation using the Opera-3D, General Particle Tracer and CST-STUDIO codes. The result of the simulation clearly shows that the role of combined functions in both the bending and the steering magnets is important for focusing the beam to a small size. FWHM sizes of the beam are predicted by simulation to be 0.45 mm (horizontal) and 0.05 mm (vertical) for a 120 keV/75 mA beam, of which the effective brilliance is about 500 kW mm−2 on the supposition of a two-dimensional Gaussian distribution. High-power tests have begun using a high-voltage 120 kV/75 mA power supply for the X-ray generator instead of 60 kV/100 mA. The beam focus size on the target will be verified in the experiments.

The pressure effect on the Nèel temperature TN of DyB6 has been investigated by measuring the temperature dependence of electrical resistivity (ρ) at various pressures up to 8 GPa. It was found that TN increases almost linearly with pressure in the range of 0-2 GPa and then tends to saturate above 2 GPa. The pressure derivative of TN below 2 GPa was estimated to be 2.6 K/GPa. The pressure effect on the volume of DyB6 has also been measured at high pressure up to 14 GPa at room temperature using X-ray diffraction and diamond anvil cell. The pressure dependence of volume of LaB6 was also measured for the comparison. It is revealed that DyB6 is more compressible than LaB6. The origin for this observation is suggested to be due to the difference of the ionic size of the rare earth elements, or the strong electron-phonon interaction in DyB6.

The distributions of CCH, C4H, c-C3H2, and HC5N have been studied in high spatial resolution with the Plateau de Bure Interferometer, where the short-spacing data have been taken with the IRAM 30 m telescope. The distributions show clear central condensation around the protostar, confirming that these molecules are associated with the protostar's environment. The blueshifted and redshifted components are concentrated near the protostar, indicating their existence in the infalling envelope. The intensity distribution of c-C3H2 shows a steep increase inward of a radius of 500-1000 AU from the protostar. By comparing the c-C3H2 distribution with the H2 column density distribution from the protostellar envelope model using the DUSTY code, the abundance of c-C3H2 is found to be enhanced by a factor of about 10 within the increasing point, where the temperature becomes higher than 20-30 K. This result supports the picture of warm carbon-chain chemistry; carbon-chain molecules and their related molecules are efficiently regenerated by evaporation of CH4 from dust grains in the warm region (about 25 K). The distributions of CCH and C4H have extended structures as well as an enhanced component, which implies a contribution of "remnant" carbon-chain molecules produced in the starless-core phase in addition to the regeneration component. On the other hand, the distributions of CCH, C4H, and c-C3H2 have a slight dip with a radius of 300-600 AU toward the protostar position, indicating that their abundances would decrease toward the central part. The present results provide a new picture of carbon-chain chemistry in the closest vicinity of a low-mass protostar.

Many indicators/indices provide information on whether the 2010 biodiversity target of reducing declines in biodiversity have been achieved. The strengths and limitations of the various measures used to assess the success of such measures are now being discussed. Biodiversity dynamics are often evaluated by a single biological population metric, such as the abundance of each species. Here we examined tree population dynamics of 52 families (192 species) at 11 research sites (three vegetation zones) of Japanese old-growth forests using two population metrics: number of stems and basal area. We calculated indices that track the rate of change in all species of tree by taking the geometric mean of changes in population metrics between the 1990s and the 2000s at the national level and at the levels of the vegetation zone and family. We specifically focused on whether indices based on these two metrics behaved similarly. The indices showed that (1) the number of stems declined, whereas basal area did not change at the national level and (2) the degree of change in the indices varied by vegetation zone and family. These results suggest that Japanese old-growth forests have not degraded and may even be developing in some vegetation zones, and indicate that the use of a single population metric (or indicator/index) may be insufficient to precisely understand the state of biodiversity. It is therefore important to incorporate more metrics into monitoring schemes to overcome the risk of misunderstanding or misrepresenting biodiversity dynamics.

We have recently discovered a new starless core with bright radio emissions of long carbon-chain molecules in the Lupus molecular cloud, which we have named as Lupus-1A. Toward this source, the peak intensities of the C6H and C8H lines are found to be higher than toward TMC-1 by a factor of 2-3. Even the lines of their anions, C6H– and C8H–, are also brighter than in TMC-1. Moreover, the line of C4H– has been detected for the first time in a starless core. The column densities of these long carbon-chain molecules are almost comparable to those in TMC-1, and hence, this source can be regarded as the second "TMC-1 like cloud." TMC-1 has long been an outstanding molecular cloud with rich carbon-chain molecules since its discovery in 1976. In spite of extensive efforts, no comparable sources have been found so far. Lupus-1A will be used for hunting of new interstellar molecules as well as understanding of carbon-chain chemistry through critical comparison of physical and chemical properties with TMC-1. This source is important not only for astronomy but also for molecular science as an ideal spectroscopic laboratory because of narrow line shapes and bright intensities.

Using Galactic Plane surveys, we have selected a massive (1200 M$_\odot$), cold (14 K) 3.6-70 $\mu$m dark IRDC G331.372-00.116. This IRDC has the potential to form high-mass stars and, given the absence of current star formation signatures, it seems to represent the earliest stages of high-mass star formation. We have mapped the whole IRDC with the Atacama Large Millimeter/submillimeter Array (ALMA) at 1.1 and 1.3 mm in dust continuum and line emission. The dust continuum reveals 22 cores distributed across the IRDC. In this work, we analyze the physical properties of the most massive core, ALMA1, which has no molecular outflows detected in the CO (2-1), SiO (5-4), and H$_2$CO (3-2) lines. This core is relatively massive ($M$ = 17.6 M$_\odot$), subvirialized (virial parameter $\alpha_{vir}=M_{vir}/M=0.14$), and is barely affected by turbulence (transonic Mach number of 1.2). Using the HCO$^+$ (3-2) line, we find the first detection of infall signatures in a relatively massive, prestellar core (ALMA1) with the potential to form a high-mass star. We estimate an infall speed of 1.54 km s$^{-1}$ and a high accretion rate of 1.96 $\times$ 10$^{-3}$ M$_\odot$ yr$^{-1}$. ALMA1 is rapidly collapsing, out of virial equilibrium, more consistent with competitive accretion scenarios rather than the turbulent core accretion model. On the other hand, ALMA1 has a mass $\sim$6 times larger than the clumps Jeans mass, being in an intermediate mass regime ($M_{J}=2.7, Comment: 13 Pages, 5 Figures, 3 Tables

Chemical diversity of the gas in low-mass protostellar cores is widely recognized. In order to explore its origin, a survey of chemical composition toward 36 Class 0/I protostars in the Perseus molecular cloud complex, which are selected in an unbiased way under certain physical conditions, has been conducted with IRAM 30 m and NRO 45 m telescope. Multiple lines of C2H, c-C3H2 and CH3OH have been observed to characterize the chemical composition averaged over a 1000 au scale around the protostar. The derived beam-averaged column densities show significant chemical diversity among the sources, where the column density ratios of C2H/CH3OH are spread out by 2 orders of magnitude. From previous studies, the hot corino sources have abundant CH3OH but deficient C2H, their C2H/CH3OH column density ratios being relatively low. In contrast, the warm-carbon-chain chemistry (WCCC) sources are found to reveal the high C2H/CH3OH column density ratios. We find that the majority of the sources have intermediate characters between these two distinct chemistry types. A possible trend is seen between the C2H/CH3OH ratio and the distance of the source from the edge of a molecular cloud. The sources located near cloud edges or in isolated clouds tend to have a high C2H/CH3OH ratio. On the other hand, the sources having a low C2H/CH3OH ratio tend to be located in inner regions of the molecular cloud complex. This result gives an important clue to an understanding of the origin of the chemical diversity of protostellar cores in terms of environmental effects., Accepted for publication in ApJS