bluuebunny/crossref_metadata_2025_split huggingface dataset:
Long‐Term Comparison of Boomerang‐Shaped Jejunal Interposition and Billroth‐I Reconstruction After Distal Gastrectomy
Authors: Sasaki Kinro , Miyachi Kazuhito , Yoda Norihito , Onodera Shinichi , Satomura Hitoshi , Otsuka Kichiro , Nakajima Masanobu , Yamaguchi Satoru , Sunagawa Masakatsu , Kato Hiroyuki 
Published: January 2015

AbstractBackgroundBillroth‐I (BI) is a simple, physiological method of reconstruction following distal gastrectomy. In actuality, postoperative QOL is by no means favorable due to the high incidence of post‐gastrectomy syndrome. The aim of this study is to assess the safety and efficacy of boomerang‐shaped jejunal interposition (BJI) after distal gastrectomy.MethodsSixty‐six patients with early gastric cancer underwent the BI procedure (n = 33) or BJI (n = 33) after distal gastrectomy, following which they were compared for 5 years. Tumor characteristics, operative details, postoperative complications and complaints, number of meals, and body weight were analyzed. Patients were followed up by endoscopy every 12 months.ResultsThere were no significant differences in the incidence of postoperative complications. The incidence of heartburn (30 vs. 0 %, P = 0.0009) and oral bitterness (33 vs. 6 %, P = 0.0112) were significantly lower in the BJI cases. Endoscopic findings revealed significantly lower incidences of reflux esophagitis (24 vs. 0 %, P = 0.0051) and remnant gastritis (70 vs. 3 %, P < 0.0001) in the BJI group. The incidence of food stasis was low in both groups (12 vs. 15 %). In the BJI group, 30 patients (90 %) were eating 3 meals/day within 12 months, whereas in the BI group, 16 patients (48 %) were still eating 5 meals/day at 12 months or later.ConclusionsBJI is as safe as BI, but is better in terms of improvement in bile reflux and food intake without stasis. This procedure, therefore, appears to be a useful method for reconstruction after distal gastrectomy.
Schistosoma Prevalence in Appendicitis
Authors: Botes S. N. , Ibirogba S. B. , McCallum A. D. , Kahn D. 
Published: January 2015

AbstractBackgroundSchistosomiasis is a waterborne trematode with numerous subtypes affecting different areas of the body. Rob Ferreira Hospital is located in an endemic area for schistosomiasis in the Lowveld region of South Africa. We set out to determine the prevalence of Schistosoma in appendicitis.MethodsFrom 2009 to 2013, all appendix samples removed in theatre were reviewed. A total of 304 cases were retrieved. Viable ova, calcified ova, or schistosomal granulomas was considered proof of exposure.ResultsThirty‐one out of the 304 cases revealed evidence of schistosomal exposure, equating to 10.2 %.ConclusionA prevalence of more than 10 % is truly significant seeing as how a delayed diagnosis can lead to serious complications, or how a misdiagnosis can result in unnecessary and often protracted treatment with harmful drugs.
Decreased production of higher alcohols by Saccharomyces cerevisiae for Chinese rice wine fermentation by deletion of Bat aminotransferases
Authors: Zhang Cui-Ying , Qi Ya-Nan , Ma Hong-Xia , Li Wei , Dai Long-Hai , Xiao Dong-Guang 
Published: January 2015

Abstract
An appropriate level of higher alcohols produced by yeast during the fermentation is one of the most important factors influencing Chinese rice wine quality. In this study, BAT1 and BAT2 single- and double-gene-deletion mutant strains were constructed from an industrial yeast strain RY1 to decrease higher alcohols during Chinese rice wine fermentation. The results showed that the BAT2 single-gene-deletion mutant strain produced best improvement in the production of higher alcohols while remaining showed normal growth and fermentation characteristics. Furthermore, a BAT2 single-gene-deletion diploid engineered strain RY1-Δbat2 was constructed and produced low levels of isobutanol and isoamylol (isoamyl alcohol and active amyl alcohol) in simulated fermentation of Chinese rice wine, 92.40 and 303.31 mg/L, respectively, which were 33.00 and 14.20 % lower than those of the parental strain RY1. The differences in fermentation performance between RY1-Δbat2 and RY1 were minor. Therefore, construction of this yeast strain is important in future development in Chinese wine industry and provides insights on generating yeast strains for other fermented alcoholic beverages.
Effects of Fuel Impingement-Cooling on the Combustion Flow in a Small Bipropellant Liquid Rocket Thruster
Authors: Lee Y.-W. , Jiang T.-L. 
Published: January 2015

ABSTRACTIn the present study, a three-dimensional computer code, based on the computer software KIVA-3, was developed for the combustion-flow simulation of a bipropellant liquid rocket thruster. A jets-impingement model is proposed for the unlike-doublet jet impingement issue. The computer code is employed to simulate a small bipropellant liquid rocket engine installed with three unlike-doublet injectors of NTO and MMH as well as six fuel injectors injecting MMH toward the combustor wall for cooling. Effects of the fuel-injection cooling on the combustion flow, combustion efficiency, and wall temperature were investigated. The results obtained from the present study show that under the present injector configuration and a constant total fuel-flow rate, higher cooling-fuel ratios make the atomized mixing flow of NTO and MMH shift toward the combustor wall, resulting in lower combustion efficiency and chamber pressure; however, low cooling-fuel ratios are unable to keep the wall-temperature sufficiently low. To overcome this issue, the proposed three-dimensional computer code calculates/locates the optimal cooling-fuel ratio that bears high combustion efficiency for a bipropellant liquid rocket combustor while keeping the chamber wall sufficiently cool.
DSMC Study of Pressure-Driven Slip Flow through Microchannel at Non-Uniform Wall Temperature
Authors: Tai C.-C. , Tzeng P.-Y. , Soong C.-Y. 
Published: January 2015

ABSTRACTThe present study is to investigate the pressure-driven gas flow in microchannel at no-uniform wall temperature. DSMC is employed to generate the flow field details which are then used in analysis of the slip flow characteristics. The major concern is the influences of thermal creep effect on the pressure-driven slip flow. Thermal creep is resulted from tangential wall temperature gradient. In this work, two kinds of thermal boundary condition are considered. One is the linearly varied temperature (LVT) applied to both walls, the other is that has the bottom wall at a thermal condition combined LVT and adiabatic (AD) wall, i.e. LVT-AD-LVT condition. The present DSMC results reveal that the fluid slip is weakened (enhanced) in the case with a negative (positive) wall temperature gradient. Relatively, thermal creep effect on fluid slip over the adiabatic wall is more pronounced in the presence of negative wall temperature gradient. The mass flowrate is a strong function of the wall temperature gradient. However, there is only little difference between the mass flowrates predicted under the two kinds of thermal conditions studied in the present work.
Effect of a high-fat diet on the hepatic expression of nuclear receptors and their target genes: relevance to drug disposition
Authors: Ghoneim Ragia H. , Ngo Sock Emilienne T. , Lavoie Jean-Marc , Piquette-Miller Micheline 
Published: January 2015

More than 1·4 billion individuals are overweight or obese worldwide. While complications often require therapeutic intervention, data regarding the impact of obesity on drug disposition are scarce. As the influence of diet-induced obesity on drug transport and metabolic pathways is currently unclear, the objective of the present study was to investigate the effect of high fat feeding for 13 weeks in female Sprague–Dawley rats on the hepatic expression of the nuclear receptors pregnane X receptor (PXR), constitutive androstane receptor (CAR), liver X receptor (LXR) and farnesoid X receptor (FXR) and several of their target genes. We hypothesised that high fat feeding would alter the gene expression of major hepatic transporters through a dysregulation of the expression of the nuclear receptors. The results demonstrated that, along with a significant increase in body fat and weight, a high-fat diet (HFD) induced a significant 2-fold increase in the expression of PXR as well as a 2-, 5- and 2·5-fold increase in the hepatic expression of the PXR target genes Abcc2, Abcb1a and Cyp3a2, respectively (P< 0·05). The expression levels of FXR were significantly increased in rats fed a HFD in addition to the increase in the expression levels of FXR target genes Abcb11 and Abcb4. The expression levels of both LXRα and LXRβ were slightly but significantly increased in rats fed a HFD, and the expression levels of their target genes Abca1 and Abcg5, but not Abcg8, were significantly increased. The expression of the nuclear receptor CAR was not significantly altered between the groups. This suggests that a HFD may induce changes in the hepatobiliary transport and metabolism of endogenous and exogenous compounds.
Cloning and characterization ofifitm1andifitm3expression during early zebrafish development
Authors: Xue Wei-Wei , Wang Huan-Nan , Wang Zhi-Meng , Qiu Meng-Xi , Che Jing , Deng Feng-Jiao , Liu Jiang-Dong 
Published: January 2015

SummaryThe family of interferon-inducible transmembrane proteins (IFITMs) plays a crucial role in inhibiting proliferation, promoting homotypic cell adhesion and mediating germ cell development. In the present study, the full-length cDNAs of zebrafishifitm1(744 bp) andifitm3(702 bp) were obtained by rapid amplification of cDNA ends (RACE). Reverse transcription polymerase chain reaction (RT-PCR) analysis showed thatifitm1mRNA was expressed in the ovary, testis, brain, muscle, liver and kidney, whileifitm3mRNA was only detected in the ovary. Based onin situhybridization,ifitm1mRNA was found to be strongly expressed in the ooplasm from stage I to stage II andifitm3mRNA was also strongly expressed in the ooplasm from stage I to stage II, furthermoreifitm3expression ultimately localized to the cortex region beneath the plasma membrane of stage IV oocytes. During development,ifitm1expression was initially detected in the enveloping layer cells and deep layer cells of shield stage embryos. Then, throughout the segmentation phase (10.25–24 hours post-fertilization (hpf)),ifitm1expression was mainly detected in the head, trunk and tail regions. Unlikeifitm1,ifitm3expression was initially detected in sphere stage embryos and was then broadly expressed throughout the embryo from the 70% epiboly stage to 24 hpf. Interestingly,ifitm3was also expressed in primordial germ cells (PGCs) from the bud stage to 24 hpf. This expression analysis indicates that zebrafishifitm1may play a critical role in early organogenesis and may perform immune or hematopoietic functions andifitm3might be necessary for PGC migration and the formation of female germ cells.
Physics of rotation: problems and challenges
Authors: Maeder Andre , Meynet Georges 
Published: January 2015

AbstractWe examine some debated points in current discussions about rotating stars: the shape, the gravity darkening, the critical velocities, the mass loss rates, the hydrodynamical instabilities, the internal mixing and N–enrichments. The study of rotational mixing requires high quality data and careful analysis. From recent studies where such conditions are fulfilled, rotational mixing is well confirmed. Magnetic coupling with stellar winds may produce an apparent contradiction, i.e. stars with a low rotation and a high N–enrichment. We point out that it rather confirms the large role of shears in differentially rotating stars for the transport processes. New models of interacting binaries also show how shears and mixing may be enhanced in close binaries which are either spun up or down by tidal interactions.
Combining observational techniques to constrain convection in evolved massive star models
Authors: Georgy C. , Saio H. , Meynet G. 
Published: January 2015

AbstractRecent stellar evolution computations indicate that massive stars in the range ~ 20-30 M⊙ are located in the blue supergiant (BSG) region of the Hertzsprung-Russell diagram at two different stages of their life: immediately after the main sequence (MS, group 1) and during a blueward evolution after the red supergiant phase (group 2). From the observation of the pulsationnal properties of a subgroup of variable BSGs (α Cyg variables), one can deduce that these stars belongs to group 2. It is however difficult to simultaneously fit the observed surface abundances and gravity for these stars, and this allows to constrain the physical processes of chemical species transport in massive stars. We will show here that the surface abundances are extremely sensitive to the physics of convection, particularly the location of the intermediate convective shell that appears at the ignition of the hydrogen shell burning after the MS. Our results show that the use of the Ledoux criterion to determine the convective regions in the stellar models leads to a better fit of the surface abundances for α Cyg variables than the Schwarzschild one.
Massive stars near the Eddington-limit, pulsations & mass-loss
Authors: Gräfener G. 
Published: January 2015

AbstractVery massive stars (in excess of ~ 100 M⊙) and massive stars in pre-SN phases at the end of their evolution are continuously approaching the Eddington limit. According to our theoretical predictions their high Eddington factors lead to a peculiar sub-photospheric structure and enhanced mass-loss. Their proximity to the Eddington limit is thus likely the reason why these objects appear as LBVs and WR stars. Here we discuss how our predictions relate to the characteristics of strange-mode pulsations, and how rotating massive stars at low metallicities can produce spectroscopic signatures that have recently been observed in a sample of star-forming galaxies at redshifts z ≈ 2 – 4.
Stellar Yields of Rotating First Stars: Yields of Weak Supernovae and Abundances of Carbon-enhanced Hyper Metal Poor Stars
Authors: Takahashi Koh , Umeda Hideyuki , Yoshida Takashi 
Published: January 2015

AbstractThe three most iron-poor stars known until now are also known to have peculiar enhancements of intermediate mass elements. Under the assumption that these iron-deficient stars reveal the nucleosynthesis result of Pop III stars, we show that a weak supernova model successfully reproduces the observed abundance patterns. Moreover, we show that the initial parameters of the progenitor, such as the initial masses and the rotational property, can be constrained by the model, since the stellar yields result from the nucleosynthesis in the outer region of the star, which is significantly affected by the initial parameters. The initial parameter of Pop III stars is of prime importance for the theoretical study of the early universe. Future observation will increase the number of such carbon enhanced iron-deficient stars, and the same analysis on the stars may give valuable information for the Pop III stars that existed in our universe.
Non-LTE Abundances in OB stars: Preliminary Results for 5 Stars in the Outer Galactic Disk
Authors: Bragançca G. A. , Lanz T. , Daflon S. , Cunha K. , Garmany C. D. , Glaspey J. W. , Borges Fernandes M. , Oey M. S. , Bensby T. , Hubeny I. 
Published: January 2015

AbstractThe aim of this study is to analyse and determine elemental abundances for a large sample of distant B stars in the outer Galactic disk in order to constrain the chemical distribution of the Galactic disk and models of chemical evolution of the Galaxy. Here, we present preliminary results on a few stars along with the adopted methodology based on securing simultaneous O and Si ionization equilibria with consistent NLTE model atmospheres.
Evolution of the rotational properties and nitrogen surface abundances of B-Type stellar populations
Authors: Granada A. , Meynet G. , Ekström S. , Georgy C. , Haemmerlé L. 
Published: January 2015

AbstractStellar evolution models predict that rotation induces the mixing of chemical species, with the subsequent surface abundance anomalies relative to single non-rotating models, even during the main sequence (MS) evolution. The lack of measurable nitrogen surface enrichment in MS rotating stars, such as Be stars, has been interpreted as being in conflict with evolutionary models (e.g. Lennon et al. 2005; Hunter et al. 2008). In order to have an insight on the kind of ambient we do or we do not expect to find enriched rotating stars, we use our new population synthesis code, to produce synthetic intermediate-mass stellar populations fully accounting for stellar rotation effects, and study their evolution in time.
Study of environment and photosphere of 51 Oph
Authors: Jamialahmadi N. , Berio Ph. , Lopez B. , Meilland A. , Stee Ph. 
Published: January 2015

AbstractThe main objective of this work is to improve our understanding of young fast-rotating stars evolving from the Herbig Ae/Be class to the Vega-like one. We observed with the VEGA instrument on CHARA one object so-called 51 Oph that is probably in such an evolutionary phase, allowing us to measure a mean stellar radius for the first time for this star and to show that the Hα emission was produced in a Keplerian rotating disc. However, additional observations are needed to improve our (u,v) plan coverage in order to measure the flattening of this close-to-critically rotating star and to probe the inner region of its circumstellar gaseous disc. These studies will help to disentangle the gas and dust emission around this late young star and will finally improve our understanding of the planet formation conditions in the inner regions of protoplanetary discs.
A Search for Hot Subdwarf Companions to Rapidly-Rotating Early B Stars
Authors: Peters Geraldine J. , Gies Douglas R. , Wang Luqian , Grundstrom Erika D. 
Published: January 2015

AbstractWe continue to search for O-type subdwarf companions in binary systems containing Be primaries. We were not able to confirm an sdO object in π Aqr and HR 2142, even though optical and UV observations suggest their presence. Some possible reasons are enumerated.
An empirical pipeline for determining the viscosity parameter for Be star disks
Authors: Rímulo Leandro R. , Carciofi Alex C. , Rivinius Thomas , Haubois Xavier 
Published: January 2015

AbstractBe star phenomenology is strongly associated with their viscous circumstellar disks. Recently, models became available for the temporal evolution of these disks when subject to variable mass ejection rates. In this contribution we will discuss how these dynamical disk models, modeled with the radiative transfer code HDUST, can be used for constraining fundamental disk parameters, such as the α viscosity parameter, and we will report on an ongoing effort to model light curves of a large number of stars.
NGC 3293 revisited by the Gaia-ESO Survey
Authors: Semaan Thierry , Morel Thierry , Gosset Eric , Zorec Juan , Frémat Yves , Blomme Ronny , Lobel Alex 
Published: January 2015

AbstractIn the framework of the Gaia-ESO survey we have determined the fundamental parameters of a large number of B-type stars in the Galactic, young open cluster NGC 3293. The determination of the stellar parameters is based on medium-resolution spectra obtained with FLAMES/GIRAFFE at ESO-VLT. As a second step, we adopted the accurate parameters to determine the chemical abundances of these hot stars. We present a comparison of our results with those obtained by the 'VLT-FLAMES survey of massive stars' (Evans et al. 2005). Our study increases the number of objects analysed and provides an extended view of this cluster.
Wolf-Rayet stars from Very Massive Stars
Authors: Yusof Norhasliza 
Published: January 2015

AbstractMany studies focused on very massive stars (VMS) within the framework of Pop. III stars, because this is where they were thought to be abundant. In this work, we focus on the evolution of VMS in the local universe following the discovery of VMS in the R136 cluster in the Large Magellanic Cloud (LMC). We computed grids of VMS evolutionary tracks in the range 120–500 M⊙ with solar, LMC and Small Magellanic Cloud metallicities. All models end their lives as Wolf-Rayet (WR) stars of the WC (or WO) type. We discuss the evolution and fate of VMS around solar metallicity with particular focus on the WR phase. For example, we show that a distinctive feature that may be used to disentangle Wolf-Rayet stars originating from VMS from those originating from lower initial masses is the enhanced abundances of Ne and Mg at the surface of WC stars.
Asteroseismology of OB stars with hundreds of single snapshot spectra (and a few time-series of selected targets)
Authors: Simón-Díaz S. 
Published: January 2015

AbstractImagine we could do asteroseismology of large samples of OB-type stars by using just one spectrum per target. That would be great! But this is probably a crazy and stupid idea. Or maybe not. Maybe we have the possibility to open a new window to investigate stellar oscillations in massive stars that has been in front of us for many years, but has not attracted very much our attention: the characterization and understanding of the so-called macroturbulent broadening in OB-type stars.
Probing high-mass stellar evolutionary models with binary stars
Authors: Tkachenko A. 
Published: January 2015

AbstractMass discrepancy is one of the problems that is pending a solution in (massive) binary star research field. The problem is often solved by introducing an additional near core mixing into evolutionary models, which brings theoretical masses of individual stellar components into an agreement with the dynamical ones. In the present study, we perform a detailed analysis of two massive binary systems, V380 Cyg and σ Sco, to provide an independent, asteroseismic measurement of the overshoot parameter, and to test state-of-the-art stellar evolution models.
Leaky-wave-induced disks around Be stars: a pulsational analysis on their formation
Authors: Godart Melanie , Shibahashi Hiromoto , Dupret Marc-Antoine 
Published: January 2015

AbstractBe stars are B-type stars near the main sequence which undergo episodic mass loss events detected by emission lines, whose line shape and intensity vary with a timescale of the order of decades. Spectroscopic observations show a large rotation velocity such that one of the prevailing scenarios for the formation of the equatorial disk consists in an increasing equatorial rotation velocity to the break-up limit where gravity is challenged by the centrifugal force. We investigate here a new scenario recently suggested by Ishimatsu & Shibahashi (2013), in which the transport of angular momentum through the photosphere would be achieved by leaky waves, keeping the rotation velocity still below the break-up limit.
Deep Photospheric Emission Lines as Probes for Pulsational Waves
Authors: Rivinius Th. , Shultz M. , Wade G. A. 
Published: January 2015

AbstractWeak line emission originating in the photosphere is well known from O stars and widely used for luminosity classification. The physical origin of the line emission are NLTE effects, most often optical pumping by far-UV lines. Analogous lines in B stars of lower luminosity are identified in radially pulsating β Cephei stars. Their diagnostic value is shown for radially pulsating stars, as these lines probe a much larger range of the photosphere than absorption lines, and can be traced to regions where the pulsation amplitude is much lower than seen in the absorption lines.