bluuebunny/crossref_metadata_2025_split huggingface dataset:
Self‐cleaning, titanium dioxide based, multilayer coating fabricated on polymer and glass surfaces
Authors: Kasanen Jussi , Suvanto Mika , Pakkanen Tuula T. 
Published: November 2008

AbstractA photocatalytic self‐cleaning titanium dioxide (TiO2) coating was prepared as a multilayer coating structure by the spin‐coating method. Three substrate materials (two thermoplastics and one ceramic) were used: (1) high‐density polyethylene (HDPE), (2) poly(vinyl chloride), and (3) borosilicate glass (BK7). The multilayer structure consisted of a polyurethane protective layer on the substrate, two layers of photocatalytic TiO2 on the protective layer, and finally immobilized TiO2 particles bound in a diluted polyurethane dispersion. Photocatalytically active surfaces were achieved by reactive oxygen‐plasma surface etching of the fabricated coatings. The structure and properties of the coating surfaces were characterized with scanning electron microscopy and contact‐angle measurements. The coatings on HDPE and BK7 were rendered superhydrophilic by an oxygen‐plasma treatment. The photocatalytic activity and self‐cleaning properties of the prepared surfaces were studied with palmitic acid (model soil), the degradation of which was confirmed by contact‐angle measurements and gas chromatography analysis. © 2008 Wiley Periodicals, Inc. J Appl Polym Sci, 2009
Mechanical behavior of agro‐residue‐reinforced polypropylene composites
Authors: Ashori Alireza , Nourbakhsh Amir 
Published: November 2008

AbstractIn this research, fully environment‐friendly, sustainable and biodegradable composites were fabricated, using wheat straw and rice husk as reinforcements for thermoplastics, as an alternative to wood fibers. Mechanical properties including tensile, flexural, and impact strength properties were examined as a function of the amount of fiber and coupling agent used. In the sample preparation, three levels of fiber loading (30, 40, and 50 wt %) and two levels of coupling agent content (0 and 2 wt %) were used. As the percentage of fiber loading increased, flexural and tensile properties increased significantly. Notched Izod results showed a decrease in strength as the percentage of fiber increases. With addition of 50% fiber, the impact strengths decreased to 16.3, 14.4, and 16.4 J/m respectively, for wheat straw‐, rice husk‐, and poplar‐filled composites. In general, presence of coupling agent had a great effect on the mechanical strength properties. Wheat straw‐ and rice husk‐filled composites showed an increase in the tensile and flexural properties with the incorporation of the coupling agent. From these results, we can conclude that wheat straw and rice husk fibers can be potentially suitable raw materials for manufacturing biocomposite products. © 2008 Wiley Periodicals, Inc. J Appl Polym Sci, 2009
Preparation of a polymeric membrane with a fine porous structure by dry casting
Authors: Kim Jae‐Kyung , Taki Kentaro , Nagamine Shinsuke , Ohshima Masahiro 
Published: November 2008

AbstractWe prepared a polymeric membrane with a fine porous structure from polystyrene (PS), poly(ethylene glycol) (PEG), and solvent solutions by exploiting the phase separation induced in the course of dry casting. To determine the effect of the drying rate and phase separation on the developed porous structure, six different solvents, including toluene, chlorobenzene, tetrahydrofuran, methyl ethyl ketone, 1,4‐dioxane, and chloroform, were used. The pore size and density drastically changed with the different solvents and drying conditions. The polymer concentration at the onset of the phase separation into PEG‐rich and PS‐rich phases also strongly affected the cellular structure. The solubility of PEG into PS and the solvent solutions changed the concentration, which corresponded to the viscosity of the PS‐rich solution at the onset of the phase separation. The higher solubility of PEG in the solutions delayed the onset of phase separation during drying and increased the viscosity. The higher viscosity and the higher drying rate prevented the phase‐separated PEG domains from coalescing and made the resulting pore size smaller and the pore density larger. The finest porous structure, with a pore size of approximately 1 μm and a pore density of 0.08 1/μm2, was prepared from PS/PEG and a 90 wt % chloroform solution. © 2008 Wiley Periodicals, Inc. J Appl Polym Sci, 2009
Legislation and the capacity for rapid‐response management of nonindigenous species of fish in contiguous waters of Canada and the USA
Authors: Thomas Vernon G. , Vásárhelyi Charlotte , NIIMI Arthur J. 
Published: November 2008

AbstractThe provision of Canadian and US hard, enforceable, law to authorize rapid response management of nonindigenous aquatic species originating from aquaculture, live fish sales, bait fish, and the pet trade was analysed at the provincial/state levels of government for the Atlantic, Laurentian Great Lakes, and Pacific regions of North America.No federal legal capacity for rapid response management exists in either country. US state legislation is generally better developed than Canadian provincial laws to manage the exotic fish trade. However, much discrepancy exists among provincial and state law regarding provisions to restrict or prohibit potentially harmful species. Aquaculture and baitfish use is generally better regulated than live fish markets and the pet fish trade in both countries. Only the state of Maine has laws authorizing rapid‐response management to control escaped exotic fish.Most species of nonindigenous fish arise from the aquarium, pet, and baitfish trades, and development of improved legislation containing provisions for rapid response management of escapees is warranted in all states and provinces.It is recommended that Canada amends the Fisheries Act to create the appropriate enabling legislation to monitor, assess risk, and deploy rapid response management of nonindigenous aquatic species, including fish that enter federal fresh and sea waters. Two recently‐introduced US Bills, S. 725 and H.R. 1350, with their explicit measures for early detection and fast action response, could, if passed into law, create provisions to control introduced nuisance species throughout North American waters. They would also create precedents for states and provinces that have most jurisdiction over aquaculture and trade in exotic fish to amend and align their laws in a complementary manner.Copyright © 2008 John Wiley & Sons, Ltd.
The Chromaffin Vesicle: Advances in Understanding the Composition of a Versatile, Multifunctional Secretory Organelle
Authors: Crivellato Enrico , Nico Beatrice , Ribatti Domenico 
Published: November 2008

AbstractChromaffin vesicles (CV) are highly sophisticated secretory organelles synthesized in adrenal medullary chromaffin cells. They contain a complex mixture of structural proteins, catecholamine neurotransmitters, peptide hormones, and the relative processing enzymes, as well as protease inhibitors. In addition, CV store ATP, ascorbic acid, and calcium. During the last decades, extensive studies have contributed to increase our understanding of the molecular composition of CV. Yet, the recent development of biochemical and imaging procedures has greatly increased the list of CV‐soluble constituents and opened new horizons as to the complexity of CV involvement in acute stress responses. Thus, a coherent picture of CV molecular composition is still to be drawn. This review article will provide a detailed account of the content of CV soluble molecules as it emerges from the most recent analytical studies. Moreover, this review article will attempt at focussing on the physiological and pathophysiological implications of the products released by CV. Anat Rec, 291:1587–1602, 2008. © 2008 Wiley‐Liss, Inc.
Requirement of TCTG(G/C) Direct Repeats and Overlapping GATA Site for Maintaining the Cardiac‐Specific Expression of Cardiac troponin T in Developing and Adult Mice
Authors: Harlan Shannon M. , Reiter Rebecca S. , Sigmund Curt D. , Lin Jenny Li‐Chun , Lin Jim Jung‐Ching 
Published: November 2008

AbstractTransgenic mouse brain shown to the right (top and bottom, dorsal and ventral views, respectively) displays an ectopic expression of LacZ transgene driven by a mutant cardiac troponin T promoter, which contains a 2‐bp substitution destroying the critical TCTG(G/C) direct repeats. In contrast, the wild type promoter drives LacZ transgene specifically in the heart (not shown) but not ectopically in the brain shown to the left (top and bottom, dorsal and ventral views, respectively). See Harlan et al., on page 1574, in this issue.
Open clusters in a dispersing molecular cloud
Authors: Chen H.‐C. , Ko C.‐M. 
Published: November 2008

AbstractStar clusters are formed in molecular clouds which are believed to be the birth places of most stars. From recent observational data, Lada & Lada (2003) estimated that only 4 to 7% of the proto‐clusters have survived. A possible reason is the dispersion of molecular clouds by UV radiation, stellar winds or supernova explosions. We study the cloud dispersion in the embedded clusters by N‐body simulations. (© 2008 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)
The turbulent ISM and the stellar IMF
Authors: Clark P.C. , Klessen R.S. 
Published: November 2008

AbstractIn this contribution, we focus on the role that turbulence can play in setting the initial mass function (IMF) of stars. Two theories are contrasted. In the first, the so‐called ‘turbulent’ fragmentation theory, the turbulence is directly responsible for breaking up the cloud into ‘cores’ which go on to form either a single star or a small N system. In such a picture, the IMF is primordial, since the mass reservoir form the young protostellar system is assumed to be set by the mass of the natal core. In the alternative picture, ‘competitive accretion’, the final mass of a protostar is determined by its position in the potential well of the cluster. As such the IMF is determined through gravitational dynamics rather than turbulence. We discuss the observation motivation for each of these cases. (© 2008 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)
High‐resolution simulations of globular cluster dynamics
Authors: Heggie D.C. , Giersz M. 
Published: November 2008

AbstractWe describe the construction of a dynamical evolutionary model of a Galactic globular cluster, using the nearby cluster M4 as an example. The method is based on a Monte Carlo code for star cluster dynamics, but includes primordial binaries and their interactions, the Galactic tide, and stellar evolution of both single and binary stars. At the age of 12 Gyr the model gives a satisfactory match to the surface brightness profile, the velocity dispersion profile, and the luminosity function in two fields. According to the model, M4 is a post‐collapse cluster, even though the surface‐brightness profile places it within the class of “King profile” clusters.We also consider the evolution of the binary population and the escape velocity from the cluster centre. Full details are given in Heggie & Giersz (2008). (© 2008 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)
Kinematics and chemical abundances ofmetal‐poor stars in the Galactic outer halo
Authors: Ishigaki M. , Chiba M. , Aoki W. 
Published: November 2008

AbstractA survey of chemical abundances for Galactic metal‐poor stars, which are likely constituents of the outer part of the halo, is currently in progress. The sample analysed so far is comprised of 26 metal‐poor ([Fe/H] < –1) stars, whose estimated orbits reach >5 kpc above and below the Galactic plane. Using these sample stars selected based on their kinematics, we carried out the high‐resolution spectroscopy with Subaru/HDS and obtained their chemical abundances. The detailed abundance pattern of the outer halo stars has important clues for the progenitor systems populating the Galactic outer halo. The current status of our survey is reported. (© 2008 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)
The Gaia project: Technique, performance and status
Authors: Jordan S. 
Published: November 2008

AbstractGaia is a satellite mission of the ESA, aiming at absolute astrometric measurements of about one billion stars (all stars down to 20th magnitude, with unprecedented accuracy. Additionally, magnitudes and colors will be obtained for all these stars, while radial‐velocities and spectral properties will be determined only for bright objects (V < 17.5). At 15th magnitude Gaia aims at an angular accuracy of 20 microarcseconds (μ as). This goal can only be reached if the geometry of the telescopes, the detectors, and the pointing of Gaia at each moment (“attitude”) can be inferred from the Gaia measurements itself with μ as accuracy. (© 2008 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)
Young star clusters in the Antennae galaxies and NGC 1487
Authors: Mengel S. , Lehnert M.D. , Thatte N. , Whitmore B. , Vacca W.D. , Chandar R. 
Published: November 2008

AbstractWe estimate the dynamical masses of several young (≈ 10 Myr) massive star clusters in two interacting galaxies, NGC 4038/4039 (“The Antennae”) and NGC 1487, under the assumption of virial equilibrium. These are compared with photometric mass estimates. A dynamical mass substantially higher than the photometric estimate could indicate non‐virial motion of the stars in the cluster, and potentially lead to cluster disruption. All but one of the Antennae clusters have dynamical and photometric mass estimates which are within a factor ≈ 2 of one another, implying both that standard IMFs provide a good approximation to the IMF of these clusters, and that there is no significant extra‐virial motion, as would be expected if they were rapidly dispersing. These results suggest that almost all of the clusters in our sample have survived the gas removal phase as bound or marginally bound objects. But a few targets (two in NGC 1487 and one in the Antennae) have Mdyn estimates which are significantly larger than the photometric mass estimates. At least two of those clusters may be actively in the process of dissolving. The dissolution candidates in both galaxies are amongst the clusters with the lowest pressures/densities measured in our sample. (© 2008 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)
High M/L ratios of UCDs: A variation of the IMF?
Authors: Mieske S. , Dabringhausen J. , Kroupa P. , Hilker M. , Baumgardt H. 
Published: November 2008

AbstractVarious studies have established that the dynamical M/L ratios of ultra‐compact dwarf galaxies (UCDs) tend to be at the limit or beyond the range explicable by standard stellar populations with canonical IMF. We discuss how IMF variations may account for these high M/L ratios and how observational approaches may in the future allow to discriminate between those possibilities. We also briefly discuss the possibility of dark matter in UCDs. (© 2008 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)
Extragalactic archeology in integrated light: A test case with NGC 4030
Authors: Ocvirk P. , Peletier R. , Lançon A. 
Published: November 2008

AbstractWe reconstruct the age‐velocity distribution of the central region of the Sbc galaxy NGC4030, by applying STECKMAP to very high qualityWHT/ISIS data.We find that the main component is a relatively young (≈2 Gyr) bulge with a ≈100 km/s velocity dispersion. The best fit solution also shows a superimposed young, kinematically cold (σv ∼ 30 km/s) component. Monte‐Carlo simulations show that the detection of this component is robust given the observational setup and quality of the data, and that it is not likely to be an artifact of the inversion procedure. We propose that this component is actually a young stellar disk, seen superimposed on the bulge. This demonstrates the feasibility of separating superimposed stellar components and measuring their age and kinematics in integrated light, thereby confirming the results of Ocvirk et al. (2006b), but this time with real data. This is an important success for our tool in a series of tests and towards new results in extragalactic archeology. (© 2008 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)
Modeling merging galaxies using MINGA: Improving restricted N‐body by dynamical friction
Authors: Petsch H.P. , Theis Ch. 
Published: November 2008

AbstractModeling interacting galaxies to reproduce observed systems is still a challenge due to the extended parameter space (among other problems). Orbit and basic galaxy parameters can be tackled by fast simulation techniques like the restricted N‐body method, applied in the fundamental work by Toomre & Toomre (1972). This approach allows today for the study of millions of models in a short time. One difficulty for the classical restricted N‐body method is the missing orbital decay, not allowing for galaxy mergers. Here we present an extension of the restricted N‐body method including dynamical friction. This treatment has been developed by a quantitative comparison with a set of self‐consistent merger simulations. By varying the dynamical friction (formalism, strength and direction), we selected the best‐fitting parameters for a set of more than 250 000 simulations. We show that our treatment reliably reproduces the orbital decay and tidal features of merging disk galaxies for mass ratios up to q = 1/3 between host and satellite. We implemented this technique into our genetic algorithm based modeling code MINGA and present first results. (© 2008 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)
APOGEE: The Apache Point Observatory Galactic Evolution Experiment
Authors: Prieto C. Allende , Majewski S.R. , Schiavon R. , Cunha K. , Frinchaboy P. , Holtzman J. , Johnston K. , Shetrone M. , Skrutskie M. , Smith V. , Wilson J. 
Published: November 2008

AbstractAPOGEE is a large‐scale, NIR, high‐resolution (R ∼ 20 000) spectroscopic survey of Galactic stars. It is one of the four experiments in SDSS‐III. Because APOGEE will observe in the H band, where the extinction is six times smaller than in V, it will be the first survey to pierce through Galactic dust and provide a vast, uniform database of chemical abundances and radial velocities for stars across all Galactic populations (bulge, disk, and halo). The survey will be conducted with a dedicated, 300‐fiber, cryogenic, spectrograph that is being built at the University of Virginia, coupled to the ARC 2.5‐m telescope at Apache Point Observatory. APOGEE will use a significant fraction of the SDSS‐III bright time during a three‐year period to observe, at high signal‐to‐noise ratio (S /N > 100), about 100 000 giant stars selected directly from 2MASS down to a typical flux limit ofH < 13. The main scientific objectives of APOGEE are: (1) measuring unbiased metallicity distributions and abundance patterns for the different Galactic stellar populations, (2) studying the processes of star formation, feedback, and chemical mixing in theMilkyWay, (3) surveying the dynamics of the bulge and disk, placing constraints on the nature and influence of the Galactic bar and spiral arms, and (4) using extensive chemodynamical data, particularly in the inner Galaxy, to unravel its formation and evolution. (© 2008 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)
A dark disc in the Milky Way
Authors: Read J.I. , Lake G. , Agertz O. , Debattista V. 
Published: November 2008

AbstractPredicting the flux of dark matter particles through the Earth is vital for current and future direct dark matter detection experiments. To date, such predictions have been based on simulations that model the dark matter alone. Here we make the first attempt to include the influence of the baryonic matter. We show that the presence of a stellar/gas disc at high redshift (z ∼ 1) causes merging satellites to be preferentially dragged towards the disc plane. This results in an accreted stellar disc, and a dark matter disc that contributes ρDDISC = 0.25–1 ρHALO at the solar position. Although not likely to be dynamically interesting, the dark disc has important implications for the direct detection of dark matter because of ist low velocity with respect to the Earth. (© 2008 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)
The construction of equilibrium phase models of stellar systems by the iterative method
Authors: Rodionov S.A. , Athanassoula E. , Sotnikova N.Ya. 
Published: November 2008

AbstractWe describe a method, called the iterative method, which can be used to construct equilibrium N ‐body models with a given mass distribution and with given kinematic properties, parameters, or constraints. This method is both very simple and very powerful and can be used for mass distributions with an arbitrary geometry and a large variety of kinematical constraints. Applications of this method include the creation of initial conditions forN ‐body simulations and the modelling of galaxies from their photometric and kinematic observations. (© 2008 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)
Peculiarities in the stellar velocity distribution of galaxies with a two‐armed spiral structure
Authors: Vorobyov E.I. , Theis Ch. 
Published: November 2008

AbstractWe expand our previous numerical study of the properties of the stellar velocity distribution within the disk of a twoarmed spiral galaxy by considering spiral stellar density waves with different global Fourier amplitudes, C2. We confirm our previous conclusion that the ratio σ1: σ2 of smallest versus largest principal axes of the stellar velocity ellipsoid becomes abnormally small near the outer edges of the stellar spiral arms. The extent to which the stellar velocity ellipsoid is elongated (as compared to the unperturbed value typical for the axisymmetric disk) increases with the strength of the spiral density wave. In particular, the C2 = 0.06 spiral can decrease the unperturbed value of σ1: σ2 by 20%, while the C2 = 0.13 spiral can decrease the unperturbed σ1: σ2 by a factor of 3. The abnormally small values of the σ1: σ2 ratio can potentially be used to track the position of stellar spiral density waves. The σϕϕ: σrr ratio is characterized by a more complex behaviour and exhibits less definite minima near the outer edges of the spiral arms. We find that the epicycle approximation is violated near the spiral arms and cannot be used in spiral galaxies with C2 ≳ 0.05–0.06 or in galaxies with the amplitude of the spiral stellar density wave (relative to the unperturbed background) of order 0.1 or greater. (© 2008 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)
Star cluster kinematics in the GAIA era
Authors: Baumgardt H. 
Published: November 2008

AbstractThe GAIA astrometric satellite will measure positions, proper motions and parallaxes of millions of stars with microarcsecond accuracy. This will greatly increase our understanding of the stellar populations of the Milky Way and their dynamics. In particular, it will be possible to determine internal and space motions of a large number of open or globular clusters with an accuracy of a few km/s or better, which will bring new insights into the way star clusters evolve and how they and the Milky Way as a whole have formed. It will also be possible to look for clusters which have a common space motion and follow tidal streams from dissolving globular clusters over many orbits by kinematically selecting their members, which will constrain the form of the galactic potential. I illustrate how GAIA will improve our knowledge on the kinematics and dynamics of star clusters and what can be learned by comparing the GAIA data with realistic N ‐body simulations of star clusters, possible with e.g. future GPU or GRAPE computers. (© 2008 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)