bluuebunny/crossref_metadata_2025_split huggingface dataset:
FIB Preparation and SEM Investigations for Three‐Dimensional Analysis of Cell Cultures on Microneedle Arrays
Authors: Friedmann A. , Cismak A. , Tautorat C. , Koester P. J. , Baumann W. , Held J. , Gaspar J. , Ruther P. , Paul O. , Heilmann A. 
Published: November 2011

SummaryWe report the investigation of the interfaces between microneedle arrays and cell cultures in patch‐on‐chip systems by using Focused Ion Beam (FIB) preparation and Scanning Electron Microscopy (SEM). First, FIB preparations of micro chips are made to determine the size and shape of the designed microneedles. In this essay, we investigate the cell‐substrate interaction, especially the cell adhesion, and the microneedle's potential cell penetration. For this purpose, cross‐sectional preparation of these hard/soft hybrid structures is performed by the FIB technology. By applying the FIB technology followed by high‐resolution imaging with SEM, new insights into the cell‐substrate interface can be received. One can clearly distinguish between cells that are only in contact with microneedles and cells that are penetrated by microneedles. A stack of slice images is collected by the application of the slice‐and‐view setup during FIB preparation and is used for threedimensional reconstruction of cells and micro‐needles. SCANNING 34: 221‐229, 2012. © 2011 Wiley Periodicals, Inc.
Optimized relay placement for wireless sensor networks federation in environmental applications
Authors: Al‐Turjman Fadi M. , Hassanein Hossam S. , Alsalih Waleed M. , Ibnkahla Mohamad 
Published: November 2011

ABSTRACTAdvances in sensing and wireless communication technologies have enabled a wide spectrum of Outdoor Environment Monitoring applications. In such applications, several wireless sensor network sectors tend to collaborate to achieve more sophisticated missions that require the existence of a communication backbone connecting (federating) different sectors. Federating these sectors is an intricate task because of the huge distances between them and because of the harsh operational conditions. A natural choice in defeating these challenges is to have multiple relay nodes (RNs) that provide vast coverage and sustain the network connectivity in harsh environments. However, these RNs are expensive; thus, the least possible number of such devices should be deployed. Furthermore, because of the harsh operational conditions in Outdoor Environment Monitoring applications, fault tolerance becomes crucial, which imposes further challenges; RNs should be deployed in such a way that tolerates failures in some links or nodes. In this paper, we propose two optimized relay placement strategies with the objective of federating disjoint wireless sensor network sectors with the maximum connectivity under a cost constraint on the total number of RNs to be deployed. The performance of the proposed approach is validated and assessed through extensive simulations and comparisons assuming practical considerations in outdoor environments. Copyright © 2011 John Wiley & Sons, Ltd.
Stented pancreaticojejunostomy (with video)
Authors: Azumi Yoshinori , Isaji Shuji 
Published: November 2011

AbstractBackground/purposeUsing a standardized technique for pancreaticojejunostomy that we term “pair‐watch suturing technique”, we prospectively analyzed the effects of a pancreatic stent tube for preventing pancreatic fistula and furthermore evaluated which perioperative factors had an influence on the development of pancreatic fistula.Operative procedureBefore anastomosis, we imagine the faces of a pair of wristwatches on the jejunal hole and pancreatic duct. The first stitch was put between 9 o'clock on the pancreatic side and 3 o'clock on the jejunal side, and a total of 7 stitches were put in the posterior wall, followed by 5 stitches in the anterior wall. Using this technique, twelve stitches can be sutured in the first layer anastomosis regardless of the caliber of the pancreatic duct.Patients and methodsFrom March 2007 to April 2009, 55 consecutive patients who underwent the pair‐watch suturing technique were divided into two groups: stent (n = 28) and no‐stent (n = 27). The incidence rate of pancreatic fistula was statistically analyzed. From March 2007 to March 2011, 102 consecutive patients were retrospectively divided into two groups according to the International Study Group on Pancreatic Fistula criteria: postoperative pancreatic fistula (POPF) and non‐POPF.ResultsPerioperative factors were almost the same between the stent and no‐stent groups, and the incidence of pancreatic fistula was very similar: 10.7% in the stent group and 14.8% in the no‐stent group. Additionally, all patients who developed pancreatic fistula belonged to grade A. Among 102 patients, 15 (14.7%) were identified as having pancreatic fistula: 9 (8.8%) in grade A, 5 (4.9%) in grade B, and 1 (0.9%) in grade C. Comparing the POPF and non‐POPF groups, we could not detect any significant risk factors for the development of pancreatic fistula.ConclusionWe consider that the pair‐watch suturing technique is less susceptible to any factors, providing reliable anastomosis for any size of pancreatic duct and any texture of remnant pancreas.
Pancreatic dissection in the procedure of pancreaticoduodenectomy (with videos)
Authors: Yamaue Hiroki , Tani Masaji , Kawai Manabu , Hirono Seiko , Okada Ken‐ichi , Miyazawa Motoki 
Published: November 2011

AbstractThe procedure of pancreaticoduodenectomy consists of three parts: resection, lymph node dissection, and reconstruction. A transection of the pancreas is commonly performed after a maneuver of the pancreatic head, exposing of the portal vein or lymph node dissection, and it should be confirmed as a safe method for pancreatic transection for decreasing the incidence of pancreatic fistula. However, there are only a few clinical trials with high levels of evidence for pancreatic surgery. In this report, we discuss the following issues: dissection of peripancreatic tissue, exposing the portal vein, pancreatic transection, dissection of the right hemicircle of the peri‐superior mesenteric artery including plexus and lymph nodes, and dissection of the pancreatic parenchyma.
The development of PCR methodology for the identification of species of the tapeworm Moniezia from cattle, goats and sheep in central Vietnam
Authors: Nguyen T.D. , Le Q.D. , Huynh V.V. , Nguyen S.T. , Nguyen T.V. , Vu-Khac H. 
Published: November 2011

AbstractThe aims of this study were to investigate the prevalence of Moniezia spp. in domestic ruminants in central Vietnam and to develop a polymerase chain reaction (PCR) technique to distinguish M. expansa from M. benedeni. Among 2040 examined domestic animals (540 cattle, 800 goats, 700 sheep) Moniezia was recovered from 5.4% of cattle, 16.4% of sheep and 20.6% of goats. A set of primers for PCR was designed to classify M. expansa and M. benedeni based on the amplification of DNA corresponding to the internal transcribed spacer of 5.8S rRNA. The 457 specimens (75 from cattle, 162 from goats, 150 from sheep, 30 from horses, 30 from chickens and 10 from dogs) were subjected to PCR for classification of Moniezia spp. PCR products with the expected sizes were amplified from bovine, ovine and caprine specimens. No specific PCR products were found for specimens from horses, chickens and dogs. Of the 75 specimens from cattle, nine were classified as M. expansa and 66 were M. benedeni. Among 162 caprine specimens, 138 were M. expansa and 24 were M. benedeni. The distribution of M. expansa and M. benedeni in 150 ovine specimens was 132 and 18, respectively. These results show that M. expansa is dominant in goats and sheep, whereas M. benedeni is more common in cattle; PCR can be used for classification of these two species.
Non-addictive psychoactive drug use: Implications for behavioral addiction
Authors: Griffiths Mark D. 
Published: November 2011

AbstractThe newly proposed framework for non-addictive psychoactive substances postulated by Müller & Schumann (M&S) provides an interesting and plausible explanation for non-addictive drug use. However, with specific reference to the relevant behavioral addiction literature, this commentary argues that the model may unexpectedly hold utility not only for non-addictive use of drugs, but also for non-addictive use of other potentially addictive behaviors.
Aspects of nicotine utilization
Authors: Warburton David M. 
Published: November 2011

AbstractThis commentary reviews the effects of nicotine on mood and cognition in support of the drug utilization concept of Müller & Schumann (M&S). Specifically, it amplifies the concept with the nicotine utilization hypothesis (NUH), which opposes the nicotine withdrawal hypothesis (NWH). Evidence against NWH comes from changes in mood after abstinence and the performance effects of nicotine supporting drug utilization.
Does drug mis-instrumentalization lead to drug abuse?
Authors: Kippin Tod E. 
Published: November 2011

AbstractUnderstanding the perceived benefits of using drugs to achieve specific mental states will provide novel insights into the reasons individuals seek to use drugs. However, the precision of attempts to instrumentalize drugs is unclear both across drugs and individuals. Moreover, mis-instrumentalization, defined as discrepancies between such endpoints, may have relevance to understanding the relation among use, abuse, and addiction.
The occurrence and the distribution of masses and radii of exoplanets
Authors: Marcy Geoffrey W. , Howard Andrew W. ,   the Kepler Team
Published: November 2011

AbstractWe analyze the statistics of Doppler-detected planets and Keplere-detected planet candidates of high integrity. We determine the number of planets per star as a function of planet mass, radius, and orbital period, and the occurrence of planets as a function of stellar mass. We consider only orbital periods less than 50 days around Solar-type (GK) stars, for which both Doppler and Kepler offer good completeness. We account for observational detection effects to determine the actual number of planets per star. From Doppler-detected planets discovered in a survey of 166 nearby G and K main sequence stars we find a planet occurrence of 15+5−4% for planets with M sin i = 3–30 ME and P < 50 d, as described in Howard et al. (2010). From Keplere, the planet occurrence is 0.130 ± 0.008, 0.023 ± 0.003, and 0.013 ± 0.002 planets per star for planets with radii 2–4, 4–8, and 8–32 RE, consistent with Doppler-detected planets. From Keplere, the number of planets per star as a function of planet radius is given by a power law, df/dlog R = kRRα with kR = 2.9+0.5−0.4, α = −1.92 ± 0.11, and R = RP/RE. Neither the Doppler-detected planets nor the Keplere-detected planets exhibit a “desert” at super-Earth and Neptune sizes for close-in orbits, as suggested by some planet population synthesis models. The distribution of planets with orbital period, P, shows a gentle increase in occurrence with orbital period in the range 2–50 d. The occurrence of small, 2–4 RE planets increases with decreasing stellar mass, with seven times more planets around low mass dwarfs (3600–4100 K) than around massive stars (6600–7100 K).
High-resolution spectroscopic view of planet formation sites
Authors: Regály Zsolt , Kiss Laszlo , Sándor Zsolt , Dullemond Cornelis P. 
Published: November 2011

AbstractTheories of planet formation predict the birth of giant planets in the inner, dense, and gas-rich regions of the circumstellar disks around young stars. These are the regions from which strong CO emission is expected. Observations have so far been unable to confirm the presence of planets caught in formation. We have developed a novel method to detect a giant planet still embedded in a circumstellar disk by the distortions of the CO molecular line profiles emerging from the protoplanetary disk's surface. The method is based on the fact that a giant planet significantly perturbs the gas velocity flow in addition to distorting the disk surface density. We have calculated the emerging molecular line profiles by combining hydrodynamical models with semianalytic radiative transfer calculations. Our results have shown that a giant Jupiter-like planet can be detected using contemporary or future high-resolution near-IR spectrographs such as VLT/CRIRES or ELT/METIS. We have also studied the effects of binarity on disk perturbations. The most interesting results have been found for eccentric circumprimary disks in mid-separation binaries, for which the disk eccentricity - detectable from the asymmetric line profiles - arises from the gravitational effects of the companion star. Our detailed simulations shed new light on how to constrain the disk kinematical state as well as its eccentricity profile. Recent findings by independent groups have shown that core-accretion is severely affected by disk eccentricity, hence detection of an eccentric protoplanetary disk in a young binary system would further constrain planet formation theories.
The visitor from an ancient galaxy: A planetary companion around an old, metal-poor red horizontal branch star
Authors: Klement Rainer J. , Setiawan Johny , Henning Thomas , Rix Hans-Walter , Rochau Boyke , Rodmann Jens , Schulze-Hartung Tim 
Published: November 2011

AbstractWe report the detection of a planetary companion around HIP 13044, a metal-poor red horizontal branch star belonging to a stellar halo stream that results from the disruption of an ancient Milky Way satellite galaxy. The detection is based on radial velocity observations with FEROS at the 2.2-m MPG/ESO telescope. The periodic radial velocity variation ofP= 16.2 days can be distinguished from the periods of the stellar activity indicators. We computed a minimum planetary mass of 1.25 Mjupand an orbital semimajor axis of 0.116 AU for the planet. This discovery is unique in three aspects: First, it is the first planet detection around a star with a metallicity much lower than few percent of the solar value; second, the planet host star resides in a stellar evolutionary stage that is still unexplored in the exoplanet surveys; third, the planetary system HIP 13044 most likely has an extragalactic origin in a disrupted former satellite of the Milky Way.
The Spitzer search for the transits of HARPS low-mass planets
Authors: Gillon Michaël , Demory Brice-Olivier , Deming Drake , Seager Sara , Lovis Christophe ,   the HARPS team
Published: November 2011

AbstractRadial velocity, microlensing and transit surveys have revealed the existence of a large population of low-mass planets in our Galaxy, the so-called ‘Super-Earths’ and ‘Neptunes’. The understanding of these objects would greatly benefit from the detection of a few of them transiting bright nearby stars, making possible their thorough characterization with high signal-to-noise follow-up measurements. Our HARPS Doppler survey has now detected dozens of low-mass planets in close orbit around bright nearby stars, and it is highly probable that a few of them do transit their host star. In this context, we have set up an ambitious Spitzer program devoted to the search for the transits of the short period low-mass planets detected by HARPS. We present here this program and some of its first results.
Physical state of the deep interior of the CoRoT-7b exoplanet
Authors: Wagner Frank W. , Sohl Frank , Rückriemen Tina , Rauer Heike 
Published: November 2011

AbstractThe present study takes the CoRoT-7b exoplanet as an analogue for massive terrestrial planets to investigate conditions, under which intrinsic magnetic fields could be sustained in liquid cores. We examine the effect of depth-dependent transport parameters (e.g., activation volume of mantle rock) on a planet's thermal structure and the related heat flux across the core mantle boundary. For terrestrial planets more massive than the Earth, our calculations suggest that a substantial part of the lowermost mantle is in a sluggish convective regime, primarily due to pressure effects on viscosity. Hence, we find substantially higher core temperatures than previously reported from parameterized convection models. We also discuss the effect of melting point depression in the presence of impurities (e.g., sulfur) in iron-rich cores and compare corresponding melting relations to the calculated thermal structure. Since impurity effects become less important at the elevated pressure and temperature conditions prevalent in the deep interior of CoRoT-7b, iron-rich cores are likely solid, implying that a self-sustained magnetic field would be absent.
The Rossiter-McLaughlin effect for exoplanets
Authors: Winn Joshua N. 
Published: November 2011

AbstractThere are now more than 35 stars with transiting planets for which the stellar obliquity—or more precisely its sky projection—has been measured, via the eponymous effect of Rossiter and McLaughlin. The history of these measurements is intriguing. For 8 years a case was gradually building that the orbits of hot Jupiters are always well-aligned with the rotation of their parent stars. Then in a sudden reversal, many misaligned systems were found, and it now seems that even retrograde systems are not uncommon. I review the measurement technique underlying these discoveries, the patterns that have emerged from the data, and the implications for theories of planet formation and migration.
Tidal evolution of star-planet systems
Authors: Mardling Rosemary A. 
Published: November 2011

AbstractThe equilibrium tide model in the weak friction approximation is used by the binary star and exoplanet communities to study the tidal evolution of short-period systems, however, each uses a slightly different approach which potentially leads to different conclusions about the timescales on which various processes occur. Here we present an overview of these two approaches, and show that for short-period planets the circularization timescales they predict differ by at most a factor of a few. A discussion of the timescales for orbital decay, spin-orbit synchronization and spin-orbit alignment is also presented.
Turning solar systems into extrasolar planetary systems in stellar clusters
Authors: Davies Melvyn B. 
Published: November 2011

AbstractMany stars are formed in some form of cluster or association. These environments can have a much higher number density of stars than the field of the galaxy. Such crowded places are hostile environments: a large fraction of initially single stars will undergo close encounters with other stars or exchange into binaries. We describe how such close encounters and exchange encounters will affect the properties of a planetary system around a single star. We define singletons as single stars which have never suffered close encounters with other stars or spent time within a binary system. It may be that planetary systems similar to our own solar system can only survive around singletons. Close encounters or the presence of a stellar companion will perturb the planetary system, leading to strong planet-planet interactions, often leaving planets on tighter and more eccentric orbits. Thus, planetary systems which initially resembled our own solar system may later more closely resemble the observed extrasolar planetary systems.
Stellar companions to exoplanet host stars with Astralux
Authors: Bergfors Carolina , Brandner Wolfgang , Henning Thomas , Daemgen Sebastian 
Published: November 2011

AbstractA close stellar companion influences the formation of planets in the system. The occurrence of stellar companions and characteristics of the stars and planets in the system provide constraints on the formation processes. We present results from our high-resolution Lucky Imaging survey for binary exoplanet host stars, including the discovery of stellar companion candidates to the transiting planet hosts WASP-12 and HAT-P-8.
Probing the impact of stellar duplicity on the frequency of giant planets: Final results of our VLT/NACO survey
Authors: Eggenberger Anne , Udry Stéphane , Chauvin Gaël , Forveille Thierry , Beuzit Jean-Luc , Lagrange Anne-Marie , Mayor Michel 
Published: November 2011

AbstractIf it is commonly agreed that the presence of a (moderately) close stellar companion affects the formation and the dynamical evolution of giant planets, the frequency of giant planets residing in binary systems separated by less than 100 AU is unknown. To address this issue, we have conducted with VLT/NACO a systematic adaptive optics search for moderately close stellar companions to 130 nearby solar-type stars. According to the data from Doppler surveys, half of our targets host at least one planetary companion, while the other half show no evidence for short-period giant planets. We present here the final results of our survey, which include a new series of second-epoch measurements to test for common proper motion. The new observations confirm the physical association of two companion candidates and prove the unbound status of many others. These results strengthen our former conclusion that circumstellar giant planets are slightly less frequent in binaries with mean semimajor axes between 35 and 100 AU than in wider systems or around single stars.
Planetesimal formation in turbulent circumstellar disks
Authors: Kirsh David , Pudritz Ralph 
Published: November 2011

AbstractPlanetesimal formation occurs early in the evolution of a solar system, embedded in the circumstellar gas disk, and it is the crucial first step in planet formation. Their growth is difficult beyond boulder size, and likely proceeds via the accumulation of many rocks in turbulence followed by gravitational collapse - a process we are only beginning to understand. We have performed global simulations of the gas disk with embedded particles in the FLASH code. Particles and gas feel drag based on differential velocities and densities. Grains and boulders of various sizes have been investigated, from micron to km, with the goal of understanding where in the disk large planetesimals will tend to form, what sizes will result, and what size ranges of grains will be preferentially incorporated. We have so far simulated particles vertical settling and radial drift under the influence of gas drag, and their accumulations in turbulent clumps.
Warm dust around ϵ Eridani
Authors: Reidemeister Martin , Krivov Alexander V. , Stark Christopher C. , Augereau Jean-Charles , Löhne Torsten , Müller Sebastian 
Published: November 2011

Abstractϵ Eridani hosts one known inner planet and an outer Kuiper belt analog. Further, Spitzer/IRS measurements indicate that warm dust is present at distances as close as a few AU from the star. Its origin is puzzling, since an “asteroid belt” that could produce this dust would be unstable because of the inner planet. We tested a hypothesis that the observed warm dust is generated by collisions in the outer belt and is transported inward by P-R drag and strong stellar winds. With numerical simulation we investigated how the dust streams from the outer ring into the inner system, and calculated the thermal emission of the dust. We show that the observed warm dust can indeed stem from the outer belt. Our models reproduce the shape and magnitude of the observed SED from mid-IR to sub-mm wavelengths, as well as the Spitzer/MIPS radial brightness profiles.
The follow-up observations for the transit events of WASP-12b
Authors: Wang Xiao-bin , Cameron Andrew Collier , Gu Sheng-hong , Fang Xiang-song , Cao Dong-tao 
Published: November 2011

AbstractThe four new transit light curves of WASP-12b are analyzed by using MCMC simulation so as to derive the system parameters. If the apsidal precession exists in the orbit of WASP-12b, according to the theory of Gimenez & Bastero (1995), the rate of precession is estimated as 0.0076 degrees per cycle in the case of orbit with an inclination of 90°.