bluuebunny/crossref_metadata_2025 huggingface dataset:
Impact of the Doping Method on Conductivity and Thermopower in Semiconducting Polythiophenes
Authors: Glaudell Anne M. , Cochran Justin E. , Patel Shrayesh N. , Chabinyc Michael L.
Published: October 2014

The development of organic semiconductors for use in thermoelectrics requires the optimization of both their thermopower and electrical conductivity. Here two fundamentally different doping mechanisms are used to investigate the thermoelectric properties of known high hole mobility polymers: poly 3‐hexylthiophene (P3HT), poly(2,5‐bis(3‐tetradecylthiophen‐2‐yl)thieno[3,2‐b]thiophene) (PBTTT‐C14), and poly(2,5‐bis(thiphen‐2‐yl)‐(3,7‐diheptadecantyltetrathienoacene)) (P2TDC17‐FT4). The small molecule tetrafluorotetracyanoquinodimethane (F4TCNQ) is known to effectively dope these polymers, and the thermoelectric properties are studied as a function of the ratio of dopant to polymer repeat unit. Higher electrical conductivity and values of the thermoelectric power factor are achieved by doping with vapor‐deposited fluoroalkyl trichlorosilanes. The combination of these data reveals a striking relationship between thermopower and conductivity in thiophene‐based polymers over a large range of electrical conductivity that is independent of the means of electrical doping. This relationship is not predicted by commonly used transport models for semiconducting polymers and is demonstrated to hold for other semiconducting polymers as well.
ADR Briefs
Authors: Shifman Bette
Published: October 2014

The US Court of Appeals for the Second Circuit has upheld two Southern District decisions in disputes concerning the proper forum for deciding claims by municipal authorities with respect to auction rate securities underwritten by Goldman.
Why Can't We Settle Disputes Like Children?
Authors: Weil Richard S.
Published: October 2014

Remember how we resolved disputes as kids? No, not the way that resulted in bloody noses. The more peaceful way, like –

Ro‐sham‐bo (Rock Paper Scissors)

Eeny‐meeny‐miny‐mo

Flipping a coin

Guess which hand the rock is in

Choosing sides or first‐ups by tossing a baseball bat

Drawing straws

One potato, two potato

Odds and evens

Arm wrestling
Cyclical behavior of solar filaments
Authors: Gao P.X. , Shi X.J. , Li Y.
Published: October 2014

The Carte Synoptique catalogue of solar filaments from 1919 March to 1957 July, corresponding to complete cycles 16‐18, is utilized to show the latitudinal migrations of solar filaments at low (≤50°) and high (>50°) latitudes and the latitudinal distributions of solar filaments for all solar filaments, solar filaments whose maximum lengths during solar disk passage are less than or equal to 70° and solar filaments whose maximum lengths during solar disk passage are larger than 70°. The results show the following. (1) The latitudinal migrations of all low‐latitude solar filaments and low‐latitude solar filaments whose maximum lengths during solar disk passage are less than or equal to 70° follow the Spörer sunspot law. However, the latitudinal migration of low‐latitude solar filaments whose maximum lengths during solar disk passage are larger than 70° do not follow the Spörer sunspot law: there is no equatorward and no poleward drift. The latitudinal migration of high‐latitude solar filaments whose maximum lengths during solar disk passage are larger than 70° is more significant than those of all high‐latitude solar filaments and high‐latitude solar filaments whose maximum lengths during solar disk passage are less than or equal to 70°: there is a poleward migration from the latitude of about 50° to 70° and an equatorward migration from the latitude of about 70° to 50° of all high‐latitude solar filaments and high‐latitude solar filaments whose maximum lengths during solar disk passage are less than or equal to 70° and there is a poleward migration from the latitude of about 50° to 80° and an equatorward migration from the latitude of about 80° to 50° of high‐latitude solar filaments whose maximum lengths during solar disk passage are larger than 70°. (2) The statistical characteristics of latitudinal distribution of solar filaments whose maximum lengths during solar disk passage are larger than 70° is different from those of all solar filaments and solar filaments whose maximum lengths during solar disk passage are less than or equal to 70° (© 2012 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)
Simulations of galaxy formation and evolution
Authors: Scannapieco C.
Published: October 2014

We discuss recent results of hydrodynamical simulations of galaxy formation in a Λ Cold Dark Matter universe, focusing on galaxies of similar mass to the Milky Way, and with a variety of formation and merger histories. We investigate the present‐day properties of disks and spheroids, in terms of stellar ages, spatial structure and dynamics; as well as the evolution of the disks. We find that disks are young, and usually composed of two or more components: the youngest stars define thinner disks that rotate ∼2 times faster than thicker disks. The latter are populated by older stars, and have 2–3 times larger velocity dispersions than the younger population. Spheroids are old and are very diverse; their inner regions are sometimes characterized by the presence of prominent bars. The disks evolve significantly during evolution. In particular, we find that major mergers and misaligned gas accretion are able to completely or partially destroy disks. These results suggest that the survival probability of disks, and therefore the final morphology of galaxies, strongly depends on the particular formation and merger history of their parent haloes. Our results show that galaxy diversity arises naturally in ΛCDM as a result of the different evolutionary paths of dark matter haloes. We also discuss the most important open problems in this field (© 2012 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)
The Bochum survey of the southern Galactic disk: I. Survey design and first results on 50 square degrees monitored in 2011
Authors: Haas M. , Hackstein M. , Ramolla M. , Drass H. , Watermann R. , Lemke R. , Chini R.
Published: October 2014

We are monitoring a 6° wide stripe along the southern Galactic disk simultaneously in the r and i bands, using a robotic 15‐cm twin telescope of the Universitätsternwarte Bochum near Cerro Armazones in Chile. Utilising the telescope's 2.7° field of view, the survey aims at observing a mosaic of 268 fields once per month and to monitor dedicated fields once per night. The survey reaches a sensitivity from 10m down to 18m (AB system), with a completeness limit of r ∼ 15.5m and i ∼ 14.5m which – due to the instrumental pixel size of 2.″4 – refers to stars separated by >3″. This brightness range is ideally suited to examine the intermediately bright stellar population supposed to be saturated in deep variability surveys with large telescopes. To connect to deep surveys or to explore faint long term variables, coadded images of several nights reach a depth of ∼ 20m. The astrometric accuracy is better than 1″, as determined from the overlap of neighbouring fields. We describe the survey design, the data properties and our procedures to derive the light curves and to extract variable stars. We present a list of ∼2200 variable stars identified in 50 square degrees with 50‐80 observations between May and October 2011. For bright stars the variability amplitude A reaches down to A ∼ 0.05m, while at the faint end variations of A > 1m are detected. About 200 stars were known tobe variable, and their amplitudes and periods – as far as determinable from our six month monitoring – agree with literature values, demonstrating the performance of the Bochum Galactic Disk Survey (© 2012 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)
Cold brown dwarfs with WISE: Y dwarfs and the field mass function
Authors: Kirkpatrick J.D.
Published: October 2014

The discovery of a new spectral class – the Y dwarfs – by NASA's Wide‐field Infrared Survey Explorer has enabled researchers to study the physics of the coldest brown dwarfs and to determine the prevalence of brown dwarfs in the Milky Way. The boundary between T dwarfs and Y dwarfs roughly coincides with the location where the J – H colors of brown dwarfs, as predicted by models, turn back to the red at effective temperatures below ∼ 400 K. Preliminary trigonometric parallax measurements show that the T/Y boundary appears also to correspond to the point at which the absolute H (1.6 µm) and W2 (4.6 µm) magnitudes plummet. Using these new distance measurements, it is found that hydrogenburning stars outnumber brown dwarfs by approximately a factor of six in the solar neighborhood. Using simulations describing the mass function as a power law or as a lognormal, we find that both the shape and predicted space densities in the mid‐T to early‐Y regime can be fit only if these functions are normalized downward to better reflect the relative paucity of brown dwarfs. The sample of currently identified Y dwarfs probes the field mass function to masses of ∼ 5 MJup, but confirmation of additional, colder Y dwarfs from WISE is needed to determine whether the low‐mass limit to star formation has yet been measured. (© 2013 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)
Multiple views of magnetism in cool stars
Authors: Morin J. , Jardine M. , Reiners A. , Shulyak D. , Beeck B. , Hallinan G. , Hebb L. , Hussain G. , Jeffers S.V. , Kochukhov O. , Vidotto A. , Walkowicz L.
Published: October 2014

Magnetic fields are regarded as a crucial element for our understanding of stellar physics. They can be studied with a variety of methods which provide complementary – and sometimes contradictory – information about the structure, strength and dynamics of the magnetic field and its role in the evolution of stars. Stellar magnetic fields can be investigated either with direct methods based on the Zeeman effect or through the observation of activity phenomena resulting from the interaction of the field with the stellar atmosphere. In this Cool Stars 17 Splinter Session we discussed the results obtained by the many ongoing studies of stellar activity and direct studies of surface magnetic fields, as well as the state‐of‐the‐art techniques on which they are based. We show the strengths and limitations of the various approaches currently used and point out their evolution as well as the interest of coupling various magnetism and activity proxies. (© 2013 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)
Multiplicity of cool dwarfs
Authors: Dupuy T.J. , Allen P.R. , Kraus A.L. , Biler B. , Blake C.H. , Davison C. , Deacon N.R. , Duchêne G. , Geller A.M. , King R.R. , Law N.M. , Nguyen D.C. , Reipurth B. , Winters J.G. , Zhang Z.H.
Published: October 2014

Multiple systems have long been used to probe the origin and evolution of stars of all masses. Only in the past 10–15 years have such studies been extended to brown dwarfs and the lowest mass stars through binary surveys of both young star forming regions and the older field population. In addition, a groundswell of interest in M dwarfs in recent years has resulted in large, modern datasets for these most common stars in the Galaxy, thereby enabling renewed perspectives on their multiplicity properties. These latest observational results have in turn fueled the many theories competing to explain the formation of low‐mass stars and brown dwarfs. This Cool Stars 17 splinter session examined the current state of this field by reviewing results from the numerous observational techniques – radial velocities, astrometry, direct imaging, and synoptic surveys – that have been used to study multiplicity from the earliest embedded protostars to objects in young star forming regions, old and intermediate‐age clusters, as well as the more heterogeneous field population. (© 2013 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)
Magnetic fields in hot stars and what we can learn for cool stars
Authors: Arlt R.
Published: October 2014

The paper focuses on the theoretical understanding of magnetic fields in radiative zones of intermediate‐mass stars. The results for magnetic instabilities and dynamo effect are then seen in view of their effects in cool stars of which in fact many also have a radiative part. We now have a detailed understanding of these magnetic instabilities and can draw first conclusions about the dynamo effect expected from them. The activity of cool stars may actually be only understandable if the dynamo process is seen in conjunction with magnetic instabilities. (© 2013 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)
Some results on the radio‐SZ correlation for galaxy cluster radio halos
Authors: Basu K.
Published: October 2014

We present correlation results for the radio halo power in galaxy clusters with the integrated thermal Sunyaev‐Zel'dovich (SZ) effect signal, including new results obtained at sub‐GHz frequencies. The radio data is compiled from several published works, and the SZ measurements are taken from the Planck ESZ cluster catalog. The tight correlation between the radio halo power and the SZ effect demonstrates a clear correspondence between the thermal and non‐thermal electron populations in the intra‐cluster medium, as already have been shown in X‐ray based studies. The radio power varies roughly as the square of the global SZ signal, but when the SZ signal is scaled to within the radio halo radius the correlation becomes approximately linear, with reduced intrinsic scatter. We do not find any strong indication of a bi‐modal division in the radio halo cluster population, as has been reported in the literature, which suggests that such duality could be an artifact of X‐ray selection. We compare the YSZ dependence of radio halos with simplified predictions from theoretical models, and discuss some implications and shortcomings of the present work. (© 2013 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)
Fundamental parameters of FR II radio galaxies and their impact on groups and clusters' environments
Authors: Kapińska A.D. , Uttley P.
Published: October 2014

Radio galaxies are among the largest and most powerful single objects known and are found at variety of redshifts, hence they are believed to have had a significant impact on the evolving Universe. Their relativistic jets inject considerable amounts of energy into the environments in which the sources reside; thus the knowledge of the fundamental properties (such as kinetic luminosities, lifetimes and ambient gas densities) of these sources is crucial for understanding AGN feedback in galaxy clusters. In this work, we explore the intrinsic and extrinsic fundamental properties of Fanaroff‐Riley II (FR II) objects through the construction of multidimensional Monte Carlo simulations which use complete, flux limited radio catalogues and semi‐analytical models of FR IIs' time evolution to create artificial samples of radio galaxies. This method allows us to set better limits on the confidence intervals of the intrinsic and extrinsic fundamental parameters and to investigate the total energy produced and injected to the clusters' environments by populations of FR IIs at various cosmological epochs (0.0 < z < 2.0). We find the latter estimates to be strikingly robust despite the strong degeneracy between the fundamental parameters – such a result points to a conclusive indicator of the scale of AGN feedback in clusters of galaxies. (© 2013 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)
The evolution of the Y –M scaling relation in MUSIC clusters
Authors: Sembolini F. , Yepes G. , De Petris M. , Gottlöber S. , Lamagna L. , Comis B.
Published: October 2014

This work describes the baryon content and Sunyaev‐Zeldovich properties of the MUSIC (Marenostrum‐MultiDark SIm‐ulations of galaxy clusters) dataset and their evolution with redshift and aperture radius. The MUSIC dataset is one of the largest samples of hydrodynamically simulated galaxy clusters (more than 2000 objects, including more than 500 clusters). We show that when the effects of cooling and stellar feedbacks are properly taken into account, the gas fraction of the MUSIC clusters consistently agrees with recent observational results. Moreover, the gas fraction has a net dependence with the total mass of the cluster and increases slightly with redshift at high overdensities.

The study of the Y –M relation confirms the consistence of the self‐similar model, showing no evolution with redshift at low overdensities. (© 2013 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)
Observability of YSOs with the WISE and AKARI infrared space observatories
Authors: Zahorecz S. , Töth L.V. , Marton G. , Ueno M. , Tamura M. , Kawamura A. , Kitamura Y.
Published: October 2014

Large area surveys allow us to identify young stellar objects and classify them based on their colours. The near‐, mid‐ and far‐infrared filters' sensitivities are different, therefore different proportions of young stars are observable. Evolutionary times for the different classes can be concluded from the popularity of the classes. Our aim was to investigate the completeness of the YSO detections. With the use of only mid‐ or only far‐infrared surveys, we will miss one part of the young stellar objects. Without far‐infrared data one third of the Class 0–II objects can remain invisible. Class III sources are almost invisible above 65 μm. For a comprehensive study we have to use the available data in the whole infrared range. (© 2013 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)
A statistical dynamical study of meteorite impactors: A case study based on parameters derived from the Bosumtwi impact event
Authors: Galiazzo M.A. , Bazsó Á. , Huber M.S. , Losiak A. , Dvorak R. , Koeberl C.
Published: October 2014

The study of meteorite craters on Earth provides information about the dynamic evolution of bodies within the Solar System. the Bosumtwi crater is a well studied, 10.5 km in diameter, ca. 1.07 Myr old impact structure located in Ghana. The impactor was ∼1 km in diameter, an ordinary chondrite and struck the Earth with an angle between 30° and 45° from the horizontal. We have used a two phase backward integration to constrain the most probable parent region of the impactor. We find that the most likely source region is a high inclination object from the Middle Main Belt. (© 2013 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)
Exploring the North‐South asymmetry in a Babcock‐Leighton dynamo
Authors: Belucz B. , Forgács‐Dajka E. , Dikpati M.
Published: October 2014

We present here a Babcock‐Leighton, kinematic flux‐transport solar dynamo model, based on an earlier model (Dikpati & Charbonneau 1999), operating in a full spherical shell of the convection zone, to investigate the properties of NorthSouth (N‐S) asymmetry. We develop a C language code for this model in order to examine the N‐S asymmetry. The main components of the model are a solar‐like internal differential rotation profile, a depth‐dependent diffusivity, and a Babcock‐Leighton type poloidal source. Our purpose here is to study what kind of North‐South asymmetry is produced in solar cycle patterns when the Babcock‐Leighton poloidal source is asymmetric between North and South. We present our solutions in the form of model butterfly diagrams in which we plot the tachocline toroidal field and surface radial field, and compare them with observations. We find that the dynamos in the northern and southern hemispheres operate nearly independently – if the Babcock‐Leighton source is much smaller in the southern hemisphere with respect to that in the northern hemisphere, the dynamo in the southern hemisphere gets weaker and weaker, but the dynamo in the northern hemisphere runs without being affected by the dynamo in the southern hemisphere. (© 2013 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)
Doppler imaging of the double‐lined active binary V824 Ara
Authors: Kriskovics L. , Vida K. , Kővári Zs. , Garcia‐Alvarez D. , Oláh K.
Published: October 2014

We introduce an iterative spectral disentangling technique combined with Doppler imaging in order to recover surface temperature maps for both components of double‐lined active binary systems. Our method provides an opportunity to separate spectra of the active components while minimizing the unwanted disturbances on the given line profile from the other component. The efficiency of the method is demonstrated on real data of the double‐lined RS CVn‐type binary V824 Ara. The resulting Doppler images reveal cool spots on the polar regions as well as low‐latitude features on both of the stars. Moreover, both components have hot spots, that are facing each other. This may indicate interconnection between the stellar magnetic fields. (© 2013 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)
Analysis of the possible Blazhko‐effect Cepheid V473 Lyrae
Authors: Molnár L. , Szabados L. , Dukes R. J. , Győrffy Á. , Szabó R.
Published: October 2014

V473 Lyrae is a peculiar Galactic Cepheid, showing strong amplitude modulation that resembles the Blazhko‐effect observed in RR Lyrae stars. We collected data spanning several modulation cycles and started a detailed analysis. The first results indicate that the star shows both amplitude and phase modulations with an average period of 1204 days, but both the cycle length and the strength of the modulation are subjected to considerable variations. A possible quintuplet component in the Fourier spectrum and additional period changes were also detected. (© 2013 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)
Elimination of long‐term variations from chaotic light curves
Authors: Plachy E. , Kolláth Z.
Published: October 2014

We performed a comparative dynamical investigation of chaotic test data using the global flow reconstruction method. We demonstrate that large‐amplitude, long‐term variations may have a disturbing effect for the analysis. The Empirical Mode Decomposition method (EMD) and the Fourier filtering were tested to remove the additional variations. Test results show that the elimination of these variations significantly increased the robustness of the reconstructions. (© 2013 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)
Hunting for binary Cepheids using the “lucky imaging” technique
Authors: Klagyivik P. , Szabados L. , Szing A. , Regály Zs.
Published: October 2014

Detecting companions to Cepheids is difficult. In most cases the brightness of the pulsator masks the fainter secondary. Since Cepheids play a key role in determining the cosmic distance scale it is crucial to find binaries among the calibrating stars of the period‐luminosity relation. Here we present an ongoing observing project of searching for faint and close companions of Galactic Cepheids using the “lucky imaging” technique. (© 2013 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)
Phase statistics of the WMAP 7 year data
Authors: Kovács A. , Szapudi I. , Frei Z.
Published: October 2014

We performed a comprehensive statistical analysis using complex phases of the alm coefficients computed from the most recent data of the Wilkinson Microwave Anisotropy Probe (WMAP). Our alm was to confirm or constrain the presence of non‐Gaussianities in the data. We found phase correlations ‐ that suggest non‐Gaussianity – at high l in alm coefficients by applying various statistical tests. Most of all, we detected a non‐Gaussian signal reaching a significance of 4.7σ using random walk statistics and simulations. However, our conclusion is that the non‐Gaussian behavior is due to contamination from galactic foregrounds that show up in small scales only. When masked out the contaminated regions, we found no significant non‐Gaussianity. Furthermore, we constrained the fNL parameter using CMB simulations that mimic primordial non‐Gaussianity. Our estimate is fNL = 40 ± 200, in agreement with previous measurements and inflationary expectations. (© 2013 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)
Supermassive black hole mergers as dual sources for electromagnetic flares in the jet emission and gravitational waves
Authors: Tápai M. , Gergely L. Á. , Keresztes Z. , Wiita P.J. , Gopal‐Krishna  , Biermann P.L.
Published: October 2014

We present a new type of observation relating the gravitational wave emission of supermassive black hole mergers to their electromagnetic counterparts. This dual emission involves variability of a relativistic jet arising from the spin‐orbit precession of the supermassive black hole binary at its base. (© 2013 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)
Synchrotron radiation of superconducting cosmic strings
Authors: Rogozin D.A. , Zadorozhna L.V.
Published: October 2014

Cosmic strings are topological defects which can be formed during the symmetry breaking phase transitions in the early Universe. Their existence finds support in modern superstring theories, both in compactification models and in theories with extended additional dimensions. Strings predicted in most grand unified models respond to external electromagnetic fields as thin superconducting wires. As they move through the cosmic magnetic fields, strings develop tremendous electric currents. Superconducting cosmic strings can serve as powerful sources of nonthermal radiation in a wide energy range, viz. as synchrotron radiation of electrons accelerated by bow shock waves which are created by the magnetosphere of strings moving relativistically through the intergalactic medium (IGM). Calculations of the expected radiation fluxes show that for typical parameters of the strings and the IGM the existing detectors can see loops at average string distances. According to our calculations they can also be observed if they are located in clusters of galaxies. (© 2013 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)
The stellar content of the young open cluster Trumpler 37
Authors: Errmann R. , Neuhäuser R. , Marschall L. , Torres G. , Mugrauer M. , Chen W.P. , Hu S.C.‐L. , Briceno C. , Chini R. , Bukowiecki Ł. , Dimitrov D.P. , Kjurkchieva D. , Jensen E.L.N. , Cohen D.H. , Wu Z.‐Y. , Pribulla T. , Vaňko M. , Krushevska V. , Budaj J. , Oasa Y. , Pandey A.K. , Fernandez M. , Kellerer A. , Marka C.
Published: October 2014

With an apparent cluster diameter of 1.5° and an age of 4 Myr, Trumpler 37 is an ideal target for photometric monitoring of young stars as well as for the search of planetary transits, eclipsing binaries and other sources of variability. The YETI consortium has monitored Trumpler 37 throughout 2010 and 2011 to obtain a comprehensive view of variable phenomena in this region. In this first paper we present the cluster properties and membership determination as derived from an extensive investigation of the literature. We also compared the coordinate list to some YETI images. For 1872 stars we found literature data. Among them 774 have high probability of being member and 125 a medium probability. Based on infrared data we re‐calculate a cluster extinction of 0.9–1.2 mag. We can confirm the age and distance to be 3–5 Myr and870 pc. Stellar masses are determined from theoretical models and the mass function is fitted with a power‐law index of α = 1.90 (0.1–0.4 M⊙) and α = 1.12 (1–10 M⊙). (© 2013 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)
Element‐abundance inhomogeneity of interstellar matter as it follows from the chemical composition of the O‐type supergiants HDE 226868 (Cyg X‐1) and α Cam
Authors: Bochkarev N.G. , Karitskaya E.A. , Shimanskii V.V. , Galazutdinov G.A.
Published: October 2014

By means of synthetic spectrum modeling with non‐LTE effects, we determined element abundances in the atmospheres of two O supergiants with similar physical characteristics: HDE 226868 (the optical component of Cyg X‐1) and α Cam. These objects are situated at the distance about 2.5 kpc from each other. HDE 226868 has higher abundances compared to α Cam. The differences of Al, S, Zn, and averaged CNO abundances are within 0.15–0.30 dex. This is in a good qualitative agreement with the inhomogeneity of the heavy‐element distribution over the Galactic disk derived by Luck et al. (2006) from Cepheids. This finding confirms the inhomogeneity of chemical‐element distribution on the scale of 2 kpc and is in agreement with the concept of interstellar‐matter superclouds preserving their intrinsic particularities on a time scale in excess of 1 Gyr. (© 2013 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)
Dense cores in the dark cloud complex LDN 1188
Authors: Verebélyi E. , Könyves V. , Nikolić S. , Kiss Cs. , Moór A. , Äbrahám P. , Kun M.
Published: October 2014

We present a molecular line emission study of the LDN 1188 dark cloud complex located in Cepheus. In this work we focused on the densest parts of the cloud and on the close neighbourhood of infrared point sources. We made ammonia mapping with the Effelsberg 100 m radio telescope and identified 3 dense cores. CS(1–0), CS(2–1) and HCO+(1–0) measurements performed with the Onsala 20 m telescope revealed the distribution of dense molecular material. The molecular line measurements were supplemented by mapping the dust emission at 1.2 mm in some selected directions using the IRAM 30 m telescope. With these data we could work out a likely evolutionary sequence in this dark cloud complex. (© 2013 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)
SOLARIS: Software for planet formation and orbital integrations
Authors: Süli Á.
Published: October 2014

I present SOLARIS a general purpose software package for doing N‐body and planet formation simulations. SOLARIS is capable to (i) to follow the orbital evolution of the solar system's major planets and minor bodies, (ii) to study the dynamics of exoplanetary systems, and (iii) to study the early and later phases of planetary formation. The process to bring bodies with different epochs to one common epoch, i.e. synchronization is implemented. Apart from the Newtonian gravitational forces, aerodynamic drag force, and type I and II migration forces are also implemented. The code also includes a nebula model. To speed up the computation, SOLARIS treats particles with different interaction properties. Several two–body events are monitored, such as collision, ejection etc. Arbitrary chemical composition can be assigned to massive bodies and during collisions the new body's composition is based on the mergers. The input is given in XML to define the parameters in a well‐structured and flexible way. SOLARIS is designed tobe versatile and easy to use, accepting initial conditions in either Cartesian coordinates or Keplerian orbital elements. (© 2013 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)
WSO‐UV project for high‐resolution spectroscopy and imaging
Authors: Sachkov M. , Shustov B. , Savanov I. , Gómez de Castro A.I.
Published: October 2014

During the last three decades, astronomers have had practically continuous access to the 100–300 nm spectral range that is unreachable with ground‐based instruments but where astro‐physical processes can be efficiently studied with unprecedented capability since the resonance lines of the most abundant atoms and ions at temperatures between 3000 and 300000 K are in the UV. The successful International Ultraviolet Explorer (IUE) observatory, Russian ASTRON mission and successor instruments such as the COS and STIS spectrographs on‐board the Hubble Space Telescope (HST) demonstrate the major impact that observations in the UV wavelength range have had on modern astronomy. The access to space‐based observatories is very limited. For the next decade, for the post‐HST era, the World Space Observatory UltraViolet (WSO‐UV) will be the only large telescope class mission for UV observations, both spectroscopic and imaging. By its potential, the WSO‐UV mission is similar to the HST, though it exceeds the HST/STIS in sensitivity by a factor 5–10, but all the observing time will be available for UV astronomy. In this paper, we briefly outline the WSO‐UV mission model, instrumentation description, science management plan as well as some of the key science issues that WSO–UV will address during its lifetime. (© 2014 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)
On the ephemeris of the eclipsing polar HU Aquarii
Authors: Schwope A.D. , Thinius B.D.
Published: October 2014

The magnetic cataclysmic variable HU Aquarii displayed pronounced quasi‐periodic modulations of its eclipse timing. These were interpreted in terms of the light‐travel time (LTT) effect caused by a circumbinary planet or planetary system. We report new photometric observations that revealed another precise eclipse timing for the October 2013 epoch, the first obtained in a high accretion state after many years in low or intermediate states. The eclipse was observed to occur earlier by 95.3 ± 2.0 s or 62.8 ± 2.0 s than expected for an assumed linear or quadratic ephemeris, respectively. The implied apparent strong evolution of the orbital period calls for a revision of the current planetary model or the planetary parameters. The object deserves further monitoring to uncover the true nature of the observed variability and to constrain the properties of the proposed planet or planetary system. The new observations prove that advanced amateur equipment can successfully be used in the growing field of planet search in wide circumbinary orbits via the LTT effect. (© 2014 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)
Mean‐field dynamos: The old concept and some recent developments
Authors: Rädler K.‐H.
Published: October 2014

This article elucidates the basic ideas of electrodynamics and magnetohydrodynamics of mean fields in turbulently moving conducting fluids. It is stressed that the connection of the mean electromotive force with the mean magnetic field and its first spatial derivatives is in general neither local nor instantaneous and that quite a few claims concerning pretended failures of the mean‐field concept result from ignoring this aspect. In addition to the mean‐field dynamo mechanisms of α2 and αΩ type several others are considered. Much progress in mean‐field electrodynamics and magnetohydrodynamics results from the test‐field method for calculating the coefficients that determine the connection of the mean electromotive force with the mean magnetic field. As an important example the memory effect in homogeneous isotropic turbulence is explained. In magnetohydrodynamic turbulence there is the possibility of a mean electromotive force that is primarily independent of the mean magnetic field and labeled as Yoshizawa effect. Despite of many efforts there is so far no convincing comprehensive theory of α quenching, that is, the reduction of the α effect with growing mean magnetic field, and of the saturation of mean‐field dynamos. Steps toward such a theory are explained. Finally, some remarks on laboratory experiments with dynamos are made. (© 2014 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)
Science with Herschel: Results from the HERITAGE project
Authors: Meixner M. , Seale J. , Roman‐Duval J. , Gordon K. , the HERITAGE Team
Published: October 2014

The Herschel Space Observatory completed its last observation on 2013 April 29 after completing 35000 astronomical observations resulting in numerous discoveries. In this review, we describe the capabilities and general scope of the Herschel mission. In particular, we review the science results from one of the open time key programs, the HERschel Inventory of The Agents of Galaxy Evolution (HERITAGE) in the Magellanic Clouds. The HERITAGE project mapped the Large Magellanic Cloud (LMC) and Small Magellanic Cloud (SMC) at 100, 160, 250, 350, and 500 μm using the SPIRE/PACS parallel mode. The total global fluxes for the LMC and SMC agree with measurements by other missions, including Planck. The HERITAGE maps of the LMC and SMC are dominated by the ISM dust emission and bear most resemblance to the tracers of ISM gas rather than the stellar content of the galaxies. The overriding science goal of HER‐ITAGE is to study the life cycle of matter as traced by dust in the LMC and SMC. The far‐infrared and submillimeter emission is an effective tracer of the interstellar medium (ISM) dust, the most deeply embedded young stellar objects (YSOs) and the dust ejected by the most massive stars which are discussed briefly in this review. The HERITAGE team has delivered the maps and source catalogs created for each of the 5 bands to the Herschel Science Center archive which will hold the legacy of Herschel. (© 2014 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)
RETRACTION: KLF8 is required for bladder cancer cell proliferation and migration
Authors: Liang Kai , Liu Tao , Chu Ning , Kang Jian , Zhang Rui , Yu Yong , Li Dongqi , Lu Dexiang
Published: October 2014

RETRACTION: Krüppel‐like factor 8 (KLF8) belongs to the Sp/KLF family of transcription factors. Recently, it is affirmed that KLF8 plays an important role in the regulation of epithelial–mesenchymal transition, which is a key process that occurs during cancer metastasis. Although the overexpression of KLF8 has been observed in several types of human cancers, the functional role of KLF8 in human bladder cancer remains unknown. Here, we investigated the effects of KLF8 knockdown on bladder cancer cell proliferation and migration in vitro. Lentivirus‐mediated small interfering RNA (siRNA) targeting KLF8 specifically downregulated its expression in T24 and BT5637 bladder cancer cells. Knockdown of KLF8 significantly inhibit cell proliferation and colony formation. Cell cycle analysis showed that knockdown of KLF8 arrested T24 cells in the G0/G1 phase. Moreover, cell migration was attenuated in T24 cells after KLF8 knockdown. Furthermore, knockdown of KLF8 resulted in a reduction in vimentin and N‐cadherin expression and an increase in β‐catenin expression. These results indicate that KLF8 plays a crucial role in proliferation and migration of bladder cancer cells, and inhibition of KLF8 by siRNA may provide a potential therapeutic approach for gene therapy in bladder cancer.
Determination of a novel nonfluorinated quinolone, nemonoxacin, in human feces and its glucuronide conjugate in human urine and feces by high‐performance liquid chromatography–triple quadrupole mass spectrometry
Authors: He Gaoli , Guo Beining , Yu Jicheng , Zhang Jing , Wu Xiaojie , Cao Guoying , Shi Yaoguo , Tsai Cheng‐yuan
Published: October 2014

Three methods were developed and validated for determination of nemonoxacin in human feces and its major metabolite, nemonoxacin acyl‐β‐ d‐glucuronide, in human urine and feces. Nemonoxacin was extracted by liquid–liquid extraction in feces homogenate samples and nemonoxacin acyl‐β‐ d‐glucuronide by a solid‐phase extraction procedure for pretreatment of both urine and feces homogenate sample. Separation was performed on a C18 reversed‐phase column under isocratic elution with the mobile phase consisting of acetonitrile and 0.1% formic acid. Both analytes were determined by liquid chromatography–tandem mass spectrometry with positive electrospray ionization in selected reaction monitoring mode and gatifloxacin as the internal standard. The lower limit of quantitation (LLOQ) of nemonoxacin in feces was 0.12 µg/g and the calibration curve was linear in the concentration range of 0.12–48.00 µg/g. The LLOQ of the metabolite was 0.0010 µg/mL and 0.03 µg/g in urine and feces matrices, while the linear range was 0.0010–0.2000 µg/mL and 0.03–3.00 µg/g, respectively. Validation included selectivity, accuracy, precision, linearity, recovery, matrix effect, carryover, dilution integrity and stability, indicating that the methods can quantify the corresponding analytes with excellent reliability. The validated methods were successfully applied to an absolute bioavailability clinical study of nemonoxacin malate capsule. Copyright © 2014 John Wiley & Sons, Ltd.
Correlations between brain structures and study time at home in healthy children: a longitudinal analysis
Authors: Asano Michiko , Taki Yasuyuki , Hashizume Hiroshi , Takeuchi Hikaru , Thyreau Benjamin , Sassa Yuko , Asano Kohei , Kawashima Ryuta
Published: October 2014

Introduction

Like sleeping and eating habits, the study habits adopted by children when they are at home are important contributors to lifestyle and they affect cognitive ability. It has recently been reported that sleeping and eating habits change the brain structure of children. However, no research on the effect of study habits at home on the brain structure of children has been conducted thus far. We investigated the effects of study habits at home on the brain structures of healthy children by examining correlations between study time at home and changes in brain structure over the course of 3 years.

Methods

We used the brain magnetic resonance images of 229 healthy children aged 5.6–18.4 years and computed the changes (time 2–time 1) in regional gray matter and white matter volume (rWMV) using voxel‐based morphometry. Whole‐brain multiple regression analysis revealed a significant positive correlation between study time at home and changes in rWMV in the right superior frontal gyrus (SFG). Behaviorally, we found a significant positive correlation between study time at home and change in the verbal comprehension index (VCI), one of the subscales of the Wechsler Intelligence Scale for Children–third edition (WISC–III).

Results and Conclusions

Given that the SFG is involved in memory control and that the VCI measures abilities related to vocabulary, our results indicate that greater SFG involvement in the memorization component of longer study times may result in greater increases in the number of axons and more axon branching and myelination, causing plastic changes in the neural network involved in memory processes.
Downregulation of NDUFB6 due to 9p24.1‐p13.3 loss is implicated in metastatic clear cell renal cell carcinoma
Authors: Narimatsu Takahiro , Matsuura Keiko , Nakada Chisato , Tsukamoto Yoshiyuki , Hijiya Naoki , Kai Tomoki , Inoue Toru , Uchida Tomohisa , Nomura Takeo , Sato Fuminori , Seto Masao , Takeuchi Ichiro , Mimata Hiromitsu , Moriyama Masatsugu
Published: October 2014

This study was conducted to clarify the genomic profiles of metastatic clear cell renal cell carcinomas (ccRCCs) and identify the genes responsible for development of metastasis. We analyzed the genomic profiles of 20 cases of primary ccRCC and their corresponding metastases using array‐based comparative genomic hybridization, and identified 32 chromosomal regions in which gene copy number alterations were detected more frequently in metastases than in the primary tumors. Among these 32 regions, 9p24.1‐p13.3 loss was the most statistically significant alteration. Furthermore, we found that patients with 9p24.1‐p13.3 loss in primary tumors exhibited significantly lower rates of recurrence‐free and cancer‐specific survival, suggesting that 9p loss in the primary tumor is a potential biomarker predicting early recurrence of metastasis. Interestingly, the genomic profiles of primary tumors with 9p loss resembled those of their corresponding metastases, though 9p loss was accumulated in the metastases derived from the primary tumors without 9p loss. Comparison of the mRNA expression levels revealed that 2 of 58 genes located at 9p24.1‐p13.3 were downregulated due to gene copy number loss in ccRCCs. An overexpression study of these two genes in ccRCC cell lines revealed that downregulation of NDUFB6 due to loss at 9p24.1‐p13.3 may confer a growth advantage on metastatic ccRCC cells. These results were confirmed by analyzing the data of 405 cases of ccRCC obtained from The Cancer Genome Atlas (TCGA). On the basis of our present data, we propose that NDUFB6 is a possible tumor suppressor of metastatic ccRCCs.
Immunohistochemical mapping of neuropeptide Y in the tree shrew brain
Authors: Ni Rong‐Jun , Shu Yu‐Mian , Luo Peng‐Hao , Fang Hui , Wang Yu , Yao Lei , Zhou Jiang‐Ning
Published: October 2014

Day‐active tree shrews are promising animals as research models for a variety of human disorders. Neuropeptide Y (NPY) modulates many behaviors in vertebrates. Here we examined the distribution of NPY in the brain of tree shrews (Tupaia belangeri chinensis) using immunohistochemical techniques. The differential distribution of NPY‐immunoreactive (‐ir) cells and fibers were observed in the rhinencephalon, telencephalon, diencephalon, mesencephalon, metencephalon, and myelencephalon of tree shrews. Most NPY‐ir cells were multipolar or bipolar in shape with triangular, fusiform, and/or globular perikarya. The densest cluster of NPY‐ir cells were found in the mitral cell layer of the main olfactory bulb (MOB), arcuate nucleus of the hypothalamus, and pretectal nucleus of the thalamus. The MOB presented a unique pattern of NPY immunoreactivity. Laminar distribution of NPY‐ir cells was observed in the MOB, neocortex, and hippocampus. Compared to rats, the tree shrews exhibited a particularly robust and widespread distribution of NPY‐ir cells in the MOB, bed nucleus of the stria terminalis, and amygdala as well as the ventral lateral geniculate nucleus and pretectal nucleus of the thalamus. By contrast, a low density of neurons were scattered in the striatum, neocortex, polymorph cell layer of the dentate gyrus, superior colliculus, inferior colliculus, and dorsal tegmental nucleus. These findings provide the first detailed mapping of NPY immunoreactivity in the tree shrew brain and demonstrate species differences in the distribution of this neuropeptide, providing an anatomical basis for the participation of the NPY system in the regulation of numerous physiological and behavioral processes. J. Comp. Neurol. 523:495–529, 2015. © 2014 Wiley Periodicals, Inc.
Digital in vivo 3D atlas of the antennal lobe of Drosophila melanogaster
Authors: Grabe Veit , Strutz Antonia , Baschwitz Amelie , Hansson Bill S. , Sachse Silke
Published: October 2014

As a model for primary olfactory perception, the antennal lobe (AL) of Drosophila melanogaster is among the most thoroughly investigated and well‐understood neuronal structures. Most studies investigating the functional properties and neuronal wiring of the AL are conducted in vivo, although so far the AL morphology has been mainly analyzed in vitro. Identifying the morphological subunits of the AL—the olfactory glomeruli—is usually done using in vitro AL atlases. However, the dissection and fixation procedure causes not only strong volumetric but also geometrical modifications; the result is unpredictable dislocation and a distortion of the AL glomeruli between the in vitro and in vivo brains. Hence, to characterize these artifacts, which are caused by in vitro processing, and to reliably identify glomeruli for in vivo applications, we generated a transgenic fly that expresses the red fluorescent protein DsRed directly fused to the presynaptic protein n‐synaptobrevin, under the control of the pan‐neuronal promotor elav to label the neuropil in the live animal. Using this fly line, we generated a digital 3D atlas of the live Drosophila AL; this atlas, the first of its kind, provides an excellent geometric match for in vivo studies. We verified the identity of 63% of AL glomeruli by mapping the projections of 34 GAL4‐lines of individual chemosensory receptor genes. Moreover, we characterized the innervation patterns of the two most frequently used GAL4‐lines in olfactory research: Orco‐ and GH146‐GAL4. The new in vivo AL atlas will be accessible online to the neuroscience community. J. Comp. Neurol. 523:530–544, 2015. © 2014 Wiley Periodicals, Inc.
Efficient Learning for Test Feature Classifier by Overlap Index List
Authors: Matsuo Yoshikazu , Takauji Hidenori , Kaneko Shun'Ichi
Published: October 2014

This paper presents a novel low cost learning algorithm for a test feature classifier by use of an overlap index list (OIL). In general, classifiers need a large amount of training data to achieve the high performance, which results in long computation times. The proposed algorithm using OIL can maintain search and check elemental combinatorial features from lower dimensions up to higher ones. Classification problems in real industrial inspection lines have been solved by the proposed algorithm, and large reductions in computation time have been obtained.
On‐Chip Manipulation of Magnetic Beads for Integrated Immunosensor
Authors: Ishikawa Tomohiro , Lee Jaesung , Miyake Ryo
Published: October 2014

The purpose of this work is in‐plane manipulation of dispersed magnetic beads on a chip. This makes an immunoassay chip that completes all its procedures on itself and eliminates any off‐chip components. A test chip was drawn in a 180 nm standard complementary metal oxide semiconductor process and tested. Beads with a diameter of 2.8 μm were diluted and applied to the chip. The chip successfully manipulated them with an affordable current down to 5 mA.