bluuebunny/crossref_metadata_2025_split huggingface dataset:
Transparentes Raumstabwerk über dem Innenhof des Berliner Reichstagspräsidentenpalais
Authors: Weller Bernhard , Reich Stefan , Ebert Jan 
Published: March 2010

AbstractDas Institut für Baukonstruktion, Technische Universität Dresden, ist maßgeblich an der Entwicklung von selbsttragenden transparenten Raumstabwerken beteiligt. Diese basieren auf stählernen Raumfachwerken, bei denen alle Stäbe der Druckebene durch in ihrer Ebene lastabtragende Verglasungen ersetzt werden. Im Jahr 2009 wurde eine erste Dachkonstruktion dieser neuartigen Bauweise über dem Innenhof des ehemaligen Berliner Reichstagspräsidentenpalais errichtet. Dabei handelt es sich um ein zweilagiges, einachsig gekrümmtes, biegesteifes Raumtragwerk mit Abmessungen von 21 m x 14 m. Der Lastabtrag der Druckkräfte in der Obergurtebene wird durch Mehrscheiben‐Isolierglas mit Scheibenabmessungen von 1,80 m x 1,26 m sichergestellt. Dieser Beitrag beschreibt das Konzept, die Tragwerksplanung, die Bauteilversuche zur Erlangung der ZiE sowie die Bauausführung.Transparent space grid structure above the inner courtyard of the Berlin palace Reichstagspräsidentenpalais. The Institute of Building Construction, Technische Universität Dresden, is decisively involved in the development of transparent space grid structures. These structures base on steel space grid structures, at which all steel members in the compression layer are replaced by in‐plane loaded glazing. In 2009, the first glass roof made of this new construction type was erected above the inner courtyard of the Berlin palace Reichstagspräsidentenpalais. The roof consists of a single curved, double layer transparent space grid structure with dimensions of 21 m x 14 m. The load transfer in the compression layer is ensured by IGU with regular dimensions of 1.80 m x 1.26 m. The contribution describes the concept, the structural design, the testing and the erection.
Knickfestigkeit und einheitliche Knickkurven für scheibenförmige Glasstützen mit Monoglasquerschnitt aus TVG und ESG
Authors: Feldmann Markus , Langosch Katharina 
Published: March 2010

AbstractErst in letzter Zeit wurden die Knick‐ und Stabilitätseigenschaften von Baugläsern näher erforscht. Dabei sind überwiegend Untersuchungen an Monoglasquerschnitten, vereinzelt auch an Verbundglasquerschnitten durchgeführt worden. Gleichwohl fehlt es bis jetzt an konsistenten technischen Regeln für die Bemessung von stabilitätsgefährdeten Glasbauteilen. Deswegen wurde vom Deutschen Stahlbauverband (DSTV) ein AiF‐Projekt aufgelegt, das Wissenslücken schließen und einheitliche Regelvorschläge zur Bemessung von stabilitätsgefährdeten Glasbauteilen geben soll. Das Projekt bezieht sich sowohl auf Knicken als auch auf Biegedrillknicken jeweils für verschiedene Belastungsarten und Querschnittsausführungen. Der vorliegende Aufsatz soll sich auf das Knicken von Glasstützen mit monolithischen Querschnitten beschränken und stellt die hierfür notwendigen Grundlagen, Experimente und Herleitungen von einheitlichen Knickspannungslinien vor.Buckling resistance and buckling curves of pane‐like glass columns with monolithic sections of heat strengthened and tempered glass. There is some knowledge on the stability behaviour of glass panes under axial loading, i.e. of their buckling stability. However, only a few investigations have been performed so far in this direction, predominantly at cross‐sections with monopanes and sporadically at cross‐sections with laminated glass. Thus a research project was initiated by the Deutscher Stahlbauverband (DSTV, German Steel Construction Association) and the German Ministry of Economics, by which the buckling of pane‐like glass columns as well as the lateral torsional buckling of glass beams, both with mono‐ and laminated sections has been thoroughly investigated, where the aforementioned problems are to be resolved. The article focuses on the results for buckling with monolithic sections of heat strengthened and tempered glass, giving buckling curves proposed by derivations and experiments.
Censored data
Authors: Gijbels Irène 
Published: March 2010

AbstractThe analysis of censored data is a major issue in survival studies. Censored data are together with truncated data, missing data, current status data, and others, among the complex data structures in which only partial information on the variable(s) of interest is available. In this article, we discuss the various types of censoring mechanisms and review the basic statistical procedures for right random censored data, including maximum likelihood estimation of parameters of the distribution, nonparametric estimation of the cumulative distribution function, and estimation of the cumulative hazard function. We briefly discuss two of the most popular regression models for censored data and review estimation under the proportional hazards model. Copyright © 2010 John Wiley & Sons, Inc.This article is categorized under:Data: Types and Structure > Traditional Statistical Data
Docosahexaenoic acid status in females of reproductive age with maple syrup urine disease
Authors: Mazer Laura M. , Yi Sarah H. L. , Singh Rani H. 
Published: March 2010

AbstractIndividuals with maple syrup urine disease (MSUD) have impaired metabolism of branched‐chain amino acids (BCAA) valine, isoleucine, and leucine. Life‐long dietary therapy is recommended to restrict BCAA intake and thus prevent poor neurological outcomes and death. To maintain adequate nutritional status, the majority of protein and nutrients are derived from synthetic BCAA‐free medical foods with variable fatty acid content. Given the restrictive diet and the importance of omega‐3 fatty acids, particularly docosahexaenoic acid (DHA), in neurological development, this study evaluated the dietary and fatty acid status of females of reproductive age with MSUD attending a metabolic camp. Healthy controls of similar age and sex were selected from existing normal laboratory data. Total lipid fatty acid concentration in plasma and erythrocytes was analyzed using gas chromatography–mass spectroscopy. Participants with MSUD had normal to increased concentrations of plasma and erythrocyte alpha linolenic acid (ALA) but significantly lower concentrations of plasma and erythrocyte docosahexaenoic acid (DHA) as percent of total lipid fatty acids compared with controls (plasma DHA: MSUD 1.03 ± 0.35, controls 2.87 ± 1.08; P = 0.001; erythrocyte DHA: MSUD 2.58 ± 0.58, controls 3.66 ± 0.80; P = 0.011). Dietary records reflected negligible or no DHA intake over the 3‐day period prior to the blood draw (range 0–2 mg). These results suggest females of reproductive age with MSUD have lower blood DHA concentrations than age‐matched controls. In addition, the presence of ALA in medical foods and the background diet may not counter the lack of preformed DHA in the diet. The implications of these results warrant further investigation.
NUTRIENT USE PATTERN IN THE IRRIGATED RICE-WHEAT CROPPING SYSTEM IN THE INDO-GANGETIC PLAINS OF HARYANA, INDIA
Authors: SINGH SHER , MALIK R. K. , DHANKAR J. S. , YADAV ASHOK , GARG RAJBIR , KAMBOJ B. R. , SHEORAN P. , LATHWAL O. P. 
Published: March 2010

SUMMARYOn-farm nutrient management practices were evaluated in the irrigated rice-wheat cropping system (RWCS) in northwestern India. Large farmers used comparatively higher doses of nutrients than small and medium farmers for both rice and wheat crops. On average, a field is treated with organic manure after every 15 years for rice and 53 years for wheat. Nitrogen use was generally more than the recommended dose for both crops. Phosphorus use in wheat was nearly as per recommendation, while in rice it was below the recommended dose. Potassium use was almost nil; however, the use of Zn (particularly in rice) is becoming common. Use of biofertilizers was negligible. Overall, farmers applied higher doses of organic manures, K, Zn and biofertilizers in rice than wheat, and there was increasing trend in their use with increase in the size of land holdings. Grain yield increased significantly with increase in the size of land holding in rice but remained almost same in wheat. This study generated comprehensive data on nutrient use pattern in the RWCS, thus providing necessary input to researchers, planners and developmental agencies who wish to enhance food security.
Crystallization and textural evolution of a closed-system magma chamber: insights from a crystal size distribution study of the Lilloise layered intrusion, East Greenland
Authors: MAGEE C. , O'DRISCOLL B. , CHAMBERS A. D. 
Published: March 2010

AbstractThe recognition that postcumulus processes significantly modify primary textures in layered mafic intrusions has thrown into question many early observations on which classical crystallization theories are based. Petrographic observations combined with quantitative textural analysis of samples from various stratigraphic levels of the Lilloise intrusion, East Greenland, demonstrate that postcumulus textural modification of cumulates, formed during the solidification of a closed system magma chamber, may be detected. Crystal size distribution (CSD) measurements of Lilloise cumulates and the resulting CSD profiles are compared to predicted theoretical closed system CSD profiles. Similarities between the measured CSD profiles and published predicted CSD profiles support Lilloise magma evolving in a closed system chamber and indicate that primary crystallization processes can be distinguished using quantitative textural techniques. Textural coarsening driven by syn-magmatic deformation is suggested to be the dominant postcumulus process affecting CSD plot morphology. CSD slope values and profiles (plot shapes) remain relatively constant for a given liquidus mineral (particularly olivine and clinopyroxene), so that the number of phases on the liquidus at any one time affects mineral modal abundances. As a result, CSDs generally exhibit overall smaller grainsizes and progressively lower nucleation densities at higher levels in the intrusion.
Parameter regimes for slow, intermediate and fast MHD shocks
Authors: DELMONT P. , KEPPENS R. 
Published: March 2010

AbstractWe investigate under which parameter regimes the magnetohydrodynamic (MHD) Rankine–Hugoniot conditions, which describe discontinuous solutions to the MHD equations, allow for slow, intermediate and fast shocks. We derive limiting values for the upstream and downstream shock parameters for which shocks of a given shock-type can occur. We revisit this classical topic in nonlinear MHD dynamics, augmenting the recent time reversal duality finding by in the usual shock frame parametrization.
Theory of particle diffusion in electrostatic turbulent plasma using extended direct-interaction approximation
Authors: TAGUCHI M. 
Published: March 2010

AbstractThe theory of particle diffusion in an electrostatic turbulent plasma is formulated by applying the direct-interaction approximation (DIA) to subensemble-averaged functions instead of conventional ensemble-averaged ones. This theory approximately incorporates the Lagrangian description into the DIA through decorrelation trajectories. The running diffusion coefficient is shown to be calculated by solving a nonlinear ordinary differential equation together with an equation for decorrelation trajectories and by averaging initial conditions at the starting point of trajectories.
Precise Li abundances in metal-poor stars: depletion in the Spite plateau
Authors: Meléndez J. , Casagrande L. , Ramírez I. , Asplund M. 
Published: March 2010

AbstractWe present Li abundances for 73 stars in the metallicity range −3.5 < [Fe/H] < −1.0 using improved IRFM temperatures (Casagrande et al. 2009) with precise E(B-V) values obtained mostly from interstellar NaI D lines, and high-quality equivalent widths (σEW ~ 3%). At all metallicities we uncover a fine-structure in the Li abundances of Spite plateau stars, which we trace to Li depletion that depends on both metallicity and mass. Models including atomic diffusion and turbulent mixing seem to reproduce the observed Li depletion assuming a primordial Li abundance ALi = 2.64 dex (MARCS models) or 2.72 (Kurucz overshooting models), in good agreement with current predictions (ALi = 2.72) from standard BBN.
Detailed analyses of three neutron-capture-rich carbon-enhanced metal-poor stars
Authors: Behara N. T. , Bonifacio P. , Ludwig H.-G. , Sbordone L. , González Hernández J. I. , Caffau E. 
Published: March 2010

AbstractApproximately 20% of very metal-poor stars ([Fe/H] < −2.0) are strongly enhanced in carbon ([C/Fe] > +1.0). Such stars are referred to as carbon-enhanced metal-poor (CEMP) stars. We present a chemical abundance analysis based on high resolution spectra acquired with UVES at the VLT of three dwarf CEMP stars: SDSS J1349-0229, SDSS J0912+0216 and SDSS J1036+1212. These very metal-poor stars, with [Fe/H] < −2.5, were selected from our ongoing survey of extremely metal-poor dwarf candidates from the SDSS.Among these CEMPs, SDSS J1349-0229 has been identified as a carbon star ([C/O] > +1.0). First and second peak s-process elements, as well as second peak r-process elements have been detected in all stars. In addition, elements from the third r-process peak were detected in one of the stars, SDSS J1036+1212. We present the abundance results of these stars in the context of neutron-capture nucleosynthesis theories.
The 9th Magnitude CEMP star BD+44°493: Origin of its Carbon Excess and Beryllium Abundance
Authors: Ito Hiroko , Aoki Wako , Honda Satoshi , Beers Timothy C. , Tominaga Nozomu 
Published: March 2010

AbstractWe performed a chemical abundance analysis of the very bright (V = 9.1) carbon-enhanced metal-poor (CEMP) star BD+44°493, which is the first star found with metallicity [Fe/H] < −3.5 and an apparent magnitude V < 12. The star is classified as a CEMP-no” subgiant, and its abundance pattern implies that a first-generation faint supernova is the most likely origin of its carbon excess. We set an very low upper limit on this star's beryllium abundance, which demonstrates that high C and O abundances do not necessarily imply high Be abundances.
Chemical abundances in planetary nebulae in three different galaxies
Authors: Peña Miriam 
Published: March 2010

AbstractWe analyze the PNe chemical behavior in three different galaxies, two dwarf irregulars and one spiral. Different behaviors are found. In the very low metallicity galaxy NGC 3109, PNe analyzed appear 0.39 dex O-richer than HII regions, while Ar/H ratio is, in average, 0.15 dex poorer. We interpret this as an evidence of significant O dredge-up in these LIMS, born in a very low metallicity environment. In NGC 6822, with a present metallicity 12+log O/H=8.06, two PN populations were found. A young one, with abundances similar to those in HII regions and an old population, with metallicities a factor of two lower. In this case no strong evidence for O dredge-up in LIMS is found. Therefore, metallicities lower than 12+log O/H =7.7 are required for an efficient O dredge-up. From our preliminary analysis of the abundances of PNe in NGC 300 we find that they are similar to the abundances in HII regions. Apparently, the PNe analyzed belong to a young population. Very similar abundance gradients, with galactocentric distance, are found for HII regions and for PNe.
Can we trust elemental abundances derived in late-type giants with the classical 1D stellar atmosphere models?
Authors: Kučinskas A. , Dobrovolskas V. , Ivanauskas A. , Ludwig H.-G. , Caffau E. , Blaževičius K. , Klevas J. , Prakapavičius D. 
Published: March 2010

AbstractWe compare the abundances of various chemical species as derived with 3D hydrodynamical and classical 1D stellar atmosphere codes in a late-type giant characterized by Teff =3640 K, log g = 1.0, [M/H]= 0.0. For this particular set of atmospheric parameters the 3D–1D abundance differences are generally small for neutral atoms and molecules but they may reach up to 0.3–0.4 dex in case of ions. The 3D–1D differences generally become increasingly more negative at higher excitation potentials and are typically largest in the optical wavelength range. Their sign can be both positive and negative, and depends on the excitation potential and wavelength of a given spectral line. While our results obtained with this particular late-type giant model suggest that 1D stellar atmosphere models may be safe to use with neutral atoms and molecules, care should be taken if they are exploited with ions.
Abundance Gradients and Chemical Evolution of Spiral Galaxies
Authors: Marcon-Uchida Monica M. , Matteucci Francesca , Costa Roberto D. D. 
Published: March 2010

AbstractThe distribution of chemical abundances and their variation in space and time are important tools to understand the chemical evolution of disks in spiral galaxies. In this work we present an one infall chemical evolution model for the Galactic disk based on an updated version of the Trieste group model. We adopted a pre enriched gas (to take into account the effect of the halo evolution), an inside-out scenario for the formation of the disk and a threshold in the surface gas density to regulate the star formation rate. The observational constraints for the solar neighbourhood were well reproduced and the spatial and time evolution of the radial abundance gradient were studied. We also used this model to reproduce the chemical evolution of some nearby spiral galaxies. The model was scaled to the disk properties of each galaxy and its dependence with the star formation efficiency and the time scale for the infalling gas into the disk were explored. Using this modified model we were able to reproduce the observed constraints available in the literature for this galaxies. The similarities and the differences between the chemical evolution of these objects and teh Milky Way are discussed to provide a basis to the understanding of the chemical evolution of disks.
Spitzer finds cosmic neon's and sulfur's sweet spot: part III, NGC 6822
Authors: Rubin R. H. , McNabb I. A. , Simpson J. P. , Dufour R. J. , Pauldrach A. W. A. , Colgan S. W. J. , Craven T. W. , Gitterman E. D. , Lo C. C. 
Published: March 2010

AbstractWe observed several H ii regions in the dwarf irregular galaxy NGC 6822 using the infrared spectrograph on the Spitzer Space Telescope. Our aim is twofold: first, to examine the neon to sulfur abundance ratio in order to determine how much it may vary and whether or not, it is fairly ‘universal’; second, to discriminate and test the predicted ionizing spectral energy distribution between various stellar atmosphere models by comparing with our derivation of the ratio of fractional ionizations involving neon and sulfur. This work extends our previous similar studies of H ii regions in M83 and M33 to lower metallicities.
The Galactic Thick Disk: An Observational Perspective
Authors: Reddy Bacham E. 
Published: March 2010

AbstractIn this review, we present a brief description of observational efforts to understand the Galactic thick disk and its relation to the other Galactic components. This review primarily focused on elemental abundance patterns of the thick disk population to understand the process or processes that were responsible for its existence and evolution. Kinematic and chemical properties of disk stars establish that the thick disk is a distinct component in the Milky Way, and its chemical enrichment and star formation histories hold clues to the bigger picture of understanding the Galaxy formation.
The Galactic thin and thick disks in the context of galaxy formation
Authors: Bensby Thomas , Feltzing Sofia 
Published: March 2010

AbstractWe have obtained high-resolution spectra and carried out a detailed elemental abundance analysis for a new sample of 899 F and G dwarf stars in the Solar neighbourhood. The results allow us to, in a multi-dimensional space consisting of stellar ages, detailed elemental abundances, and full kinematic information for the stars, study and trace their respective origins. Here we briefly address selection criteria and discuss how to define a thick disc star. The results are discussed in the context of galaxy formation.
Chemical similarities between the Galactic bulge and local thick disk red giant stars: analysis from optical data
Authors: Alves-Brito Alan , Meléndez Jorge , Asplund Martin 
Published: March 2010

AbstractThe Galactic structure and composition remain as one of the greatest open problems in modern astrophysics. We show here that there are chemical similarities between the Galactic bulge and local thick disk red giant stars. This finding puts strong constraints on the IMF, SFR and chemical enrichment timescale of the bulge and thick disk. Our results are based upon a detailed elemental abundance analysis of 80 high S/N and high resolution optical spectra of giant stars, in the range −1.5 < [Fe/H] < +0.5.
Atmospheric Parameters and Chemical Abundances for Herbig Ae stars
Authors: Castilho Bruno V. , Daflon Simone , Sartori Marília J. , Przybilla Norbert 
Published: March 2010

AbstractIn this work, we present temperature, surface gravity, metallicity, microturbulence and element abundances, determined from a detailed spectroscopic analysis for a sample of 9 Herbig Ae stars, based on high resolution, high S/N spectra.
On The Physical Existence of The Zeta Reticuli Moving Group: A Chemical Composition Analysis
Authors: Ferreira Letícia D. , de Mello Gustavo F. Porto , da Silva Licio 
Published: March 2010

AbstractWe report the spectroscopic analysis of six kinematical members of the Zeta Reticuli Moving Group, one of them for the first time. We confirm the existence of the Group by establishing a common abundance pattern for four kinematical members. High resolution spectra yielded abundances of Si, Ca, Fe, Ni and Ba, and others. Effective temperatures were derived from the excitation & ionization equilibria of Fe lines of four stars. For these, and the remaining two members, temperatures were derived from colors and the fitting of theoretical spectra to the Hα line, and ages and masses were estimated from theoretical HR diagrams. We suggest that the Group is physical being metal-poor and ~6 Gyr old.
Chemical Fingerprinting and Chemical Analysis of Galactic Halo Substructure
Authors: Majewski Steven R. , Chou Mei-Yin , Cunha Katia , Smith Verne V. , Patterson Richard J. , Martínez-Delgado David 
Published: March 2010

AbstractWe present high-resolution spectroscopic measurements of the abundances of the α-like element titanium (Ti) and s-process elements yttrium (Y) and lanthanum (La) for M giant candidates of (a) the Sagittarius (Sgr) dwarf spheroidal + tidal tail system, (b) the Triangulum-Andromeda (TriAnd) Star Cloud, and (c) the Galactic Anticenter Stellar Structure (GASS, or Monoceros Stream). All three systems show abundance patterns unlike the Milky Way but typical of dwarf galaxies. The Sgr system abundance patterns resemble those of the Large Magellanic Cloud. GASS/Mon chemically resembles Sgr but is distinct from TriAnd, a result that does not support previous suggestions that TriAnd is a piece of the Monoceros Stream.
FEROS Abundance Analysis of 21 Bulgelike SMR Stars
Authors: Trevisan Marina , Barbuy Beatriz , Grenon M. , Gustafsson B. , Pompéia L. 
Published: March 2010

AbstractWe analyze a sample of 21 super-metal-rich (SMR) stars, using high-resolution échelle spectra obtained with the Fiber-fed Extended Range Optical Spectrograph at the 1.5m ESO telescope. The metallicities are in the range 0.07 ≤ [Fe/H] ≤ 0.45, 3 of them in common with Pompéia et al. (2009). Geneva photometry, astrometric data from Hipparcos, and radial velocities from CORAVEL are available for these stars. The peculiar kinematics suggests the thin disk close to the bulge as the probable birthplace of these stars (Grenon 1999). From Hipparcos data, it appears that the turnoff of this population indicates an age of 10-11 Gyr (Grenon 1999). Detailed analysis of the sample stars is carried out, and atmospheric parameters are derived from spectroscopic and photometric determinations. Oxygen abundances of these stars are derived, and [O/Fe] overabundances up to +0.35 are found.