bluuebunny/crossref_metadata_2025_split huggingface dataset:
Characterization of Ultra Thin Copper Layers
Authors: Karasahin S. , Dammasch M. 
Published: August 2016

Abstract
The technological progress of microelectronic devices is directly coupled with the ability to produce transistor circuits and interconnects on the wafer level with increasingly small dimensions while providing equal or even better electrical properties and functionality. Therefore every new generation of microchip manufacturing is a challenge for the existing production technologies to compete with the raised requirements as well as for the material scientific methods to characterize and control the properties of the incorporated dielectrics and deposited metal layers with dimensions in the nm range. The following article will illustrate the investigation methods that have been applied for the development of electrolessly plated copper layers of less than 3 nm thickness to provide a conductive copper seed for subsequent copper electroplating to fill Dual Damascene interconnects of the 14 nm or 10 nm technology node. The methods used are AFM, Ellipsometry, 4-point resistivity, XPS, EELS, XRF, XRD, FIB/HR-STEM, HR-TEM.
New insights on the origin of the woody flora of the Chihuahuan Desert: The case of Lindleya
Authors: Marilyn Vásquez‐Cruz , Victoria Sosa 
Published: August 2016

PREMISE OF THE STUDY:We reconstructed aspects of the evolutionary history of Lindleya, a shrubby element in the rose family, as a model for identifying the ancestral area of the biota of the Chihuahuan Desert and for understanding the effect that pre‐Pleistocene or Pleistocene climate fluctuations had on the evolution of the plants of this desert.METHODS:We conducted phylogenetic, biogeographic, and phylogeographic analyses based on one nuclear DNA and two plastid markers sequenced for 20 populations comprising 153 accessions and representing the species’ entire distribution range. We carried out ecological niche modeling to forecast Lindleya's potential distribution under Current, Last Interglacial, and Last Glacial Maximum conditions.KEY RESULTS:The ancestral area of Lindleya populations was probably in the central and southern parts of the Chihuahuan Desert. Levels of genetic and haplotype variation were the highest in the northernmost and southernmost areas and low levels of genetic variation in the central part. Extended Bayesian skyline plots including all populations identified a slight demographic expansion ∼1 Ma. The predicted potential distribution during the Last Glacial Maximum was very restricted.CONCLUSIONS:We suggest that pre‐Pleistocene changes had an influence on the divergence of Lindleya populations. We also suggest that the ancestral area for Lindleya was the Chihuahuan Desert and that the uplift of the Trans‐Mexican Volcanic Belt isolated the Tehuacán Valley populations. Genetic and demographic analyses as well as and ecological niche modeling indicate that populations of Lindleya experienced genetic bottlenecks and that they have expanded since the Last Glacial Maximum.
NEAR-INFRARED CIRCULAR AND LINEAR POLARIMETRY OF MONOCEROS R2
Authors: Kwon Jungmi , Tamura Motohide , Hough James H. , Nagata Tetsuya , Kusakabe Nobuhiko 
Published: August 2016

ABSTRACT
We have conducted simultaneous JHK

s
-band imaging circular and linear polarimetry of the Monoceros R2 (Mon R2) cluster. We present results from deep and wide near-infrared linear polarimetry of the Mon R2 region. Prominent and extended polarized nebulosities over the Mon R2 field are revisited, and an infrared reflection nebula associated with the Mon R2 cluster and two local reflection nebulae, vdB 67 and vdB 69, is detected. We also present results from deep imaging circular polarimetry in the same region. For the first time, the observations show relatively high degrees of circular polarization (CP) in Mon R2, with as much as approximately 10% in the K

s
band. The maximum CP extent of a ring-like nebula around the Mon R2 cluster is approximately 0.60 pc, while that of a western nebula, around vdB 67, is approximately 0.24 pc. The extended size of the CP is larger than those seen in the Orion region around IRc2, while the maximum degree of CP of ∼10% is smaller than those of ∼17% seen in the Orion region. Nonetheless, both the CP size and degree of this region are among the largest in our infrared CP survey of star-forming regions. We have also investigated the time variability of the degree of the polarization of several infrared sources and found possible variations in three sources.
II ZWICKY 23 AND FAMILY: A GROUP IN INTERACTION
Authors: Wehner Elizabeth M. H. , Gallagher III John S. , Cigan Phillip J. , Rudie Gwen C. 
Published: August 2016

ABSTRACT
II Zw 23 (UGC 3179) is a luminous (M

B
∼ −21) nearby compact narrow emission line starburst galaxy with blue optical colors and strong emission lines. We present a photometric and morphological study of II Zw 23 and its interacting companion, KPG103a, using data obtained with the WIYN 3.5 m telescope in combination with a WFPC2 image from the Hubble Space Telescope archives. II Zw 23 has a highly disturbed outer structure with long trails of debris that may be contributing material toward the production of tidal dwarfs. Its central regions appear disky, a structure that is consistent with the overall rotation pattern observed in the Hα velocity field measured from Densepak observations obtained with WIYN. We find additional evidence for interaction in this system, including the discovery of a new tidal loop extending from an associated dwarf galaxy, which appears to be in the process of disrupting along its orbit. We also present Hα equivalent widths and discuss the relative star formation rates across this interacting system.
DICKE’S SUPERRADIANCE IN ASTROPHYSICS. II. THE OH 1612 MHz LINE
Authors: Rajabi Fereshteh , Houde Martin 
Published: August 2016

ABSTRACT
We apply the concept of superradiance that was introduced by Dicke in 1954 to the OH molecule 1612 MHz spectral line, which is often used for the detection of masers in the circumstellar envelopes of evolved stars. Because the detection of 1612 MHz OH masers in the outer shells of envelopes of these stars implies the existence of a population inversion and a high level of velocity coherence, and that these are two necessary requirements for superradiance, we investigate whether superradiance can also happen in these regions. Superradiance is characterized by high-intensity, spatially compact, burst-like features taking place over timescales on the order of seconds to years, depending on the size and physical conditions present in the regions harboring such sources of radiation. Our analysis suggests that superradiance provides a valid explanation for previous observations of intensity flares detected in that spectral line for the U Orionis Mira star and the IRAS 18276-1431 preplanetary nebula.
A HOT BIG BANG THEORY: MAGNETIC FIELDS AND THE EARLY EVOLUTION OF THE PROTOLUNAR DISK
Authors: Gammie C. F. , Liao Wei-Ting , Ricker P. M. 
Published: August 2016

ABSTRACT
The leading theory for the formation of Earth’s Moon invokes a collision between a Mars-sized body and the proto-Earth to produce a disk of orbiting material that later condenses to form the Moon. We show that the disk opacity is large, and cooling is therefore inefficient (

). In this regime, angular momentum transport in the disk leads to steady heating unless

. Following earlier work by Charnoz and Michaut, and Carballido et al., we show that once the disk is completely vaporized it is well coupled to the magnetic field. We consider a scenario in which turbulence driven by magnetic fields leads to a brief, hot phase where the disk is geometrically thick, with strong turbulent mixing. The disk cools by spreading until it decouples from the field. We point out that approximately half the accretion energy is dissipated in the boundary layer where the disk meets the Earth’s surface. This creates high entropy material close to the Earth, driving convection and mixing. Finally, a hot magnetized disk could drive bipolar outflows that remove mass and angular momentum from the Earth–Moon system.
CRITICAL DIFFERENCES OF ASYMMETRIC MAGNETIC RECONNECTION FROM STANDARD MODELS
Authors: Nitta S. 新田伸也 , Wada T. 和田智秀 , Fuchida T. 淵田泰介 , Kondoh K. 近藤光志 
Published: August 2016

ABSTRACT
We have clarified the structure of asymmetric magnetic reconnection in detail as the result of the spontaneous evolutionary process. The asymmetry is imposed as ratio k of the magnetic field strength in both sides of the initial current sheet (CS) in the isothermal equilibrium. The MHD simulation is carried out by the HLLD code for the long-term temporal evolution with very high spatial resolution. The resultant structure is drastically different from the symmetric case (e.g., the Petschek model) even for slight asymmetry k = 2. (1) The velocity distribution in the reconnection jet clearly shows a two-layered structure, i.e., the high-speed sub-layer in which the flow is almost field aligned and the acceleration sub-layer. (2) Higher beta side (HBS) plasma is caught in a lower beta side plasmoid. This suggests a new plasma mixing process in the reconnection events. (3) A new large strong fast shock in front of the plasmoid forms in the HBS. This can be a new particle acceleration site in the reconnection system. These critical properties that have not been reported in previous works suggest that we contribute to a better and more detailed knowledge of the reconnection of the standard model for the symmetric magnetic reconnection system.
CARBON STARS FROM LAMOST DR2 DATA
Authors: Ji Wei , Cui Wenyuan , Liu Chao , Luo Ali , Zhao Gang , Zhang Bo 
Published: August 2016

ABSTRACT
In this work, we present the new catalog of carbon stars from the LAMOST DR2 catalog. In total, 894 carbon stars are identified from multiple line indices measured from the stellar spectra. We are able to identify the carbon stars by combining the CN bands in the red end with C2 and other lines. Moreover, we also classify the carbon stars into spectral sub-types of C–H, C–R, and C–N. These sub-types show distinct features in the multi-dimensional line indices, implying that in the future they can be used to identify carbon stars from larger spectroscopic data sets. While the C–N stars are clearly separated from the others in the line index space, we find no clear separation between the C–R and C–H sub-types. The C–R and C–H stars seem to smoothly transition from one to another. This may hint that the C–R and C–H stars may not be different in their origins, instead their spectra look different because of different metallicities. Due to the relatively low spectral resolution and lower signal-to-noise ratio, the ratio of 12C/13C is not measured and thus the C–J stars are not identified.
DISCO: A 3D MOVING-MESH MAGNETOHYDRODYNAMICS CODE DESIGNED FOR THE STUDY OF ASTROPHYSICAL DISKS
Authors: Duffell Paul C. 
Published: August 2016

ABSTRACT
This work presents the publicly available moving-mesh magnetohydrodynamics (MHD) code DISCO. DISCO is efficient and accurate at evolving orbital fluid motion in two and three dimensions, especially at high Mach numbers. DISCO employs a moving-mesh approach utilizing a dynamic cylindrical mesh that can shear azimuthally to follow the orbital motion of the gas. The moving mesh removes diffusive advection errors and allows for longer time-steps than a static grid. MHD is implemented in DISCO using an HLLD Riemann solver and a novel constrained transport (CT) scheme that is compatible with the mesh motion. DISCO is tested against a wide variety of problems, which are designed to test its stability, accuracy, and scalability. In addition, several MHD tests are performed which demonstrate the accuracy and stability of the new CT approach, including two tests of the magneto-rotational instability, one testing the linear growth rate and the other following the instability into the fully turbulent regime.
A SOLAR-PUMPED FLUORESCENCE MODEL FOR LINE-BY-LINE EMISSION INTENSITIES IN THE B–X, A–X, AND X–X BAND SYSTEMS OF 12C14N
Authors: Paganini L. , Mumma M. J. 
Published: August 2016

ABSTRACT
We present a new quantitative model for detailed solar-pumped fluorescent emission of the main isotopologue of CN. The derived fluorescence efficiencies permit estimation and interpretation of ro-vibrational infrared line intensities of CN in exospheres exposed to solar (or stellar) radiation. Our g-factors are applicable to astronomical observations of CN extending from infrared to optical wavelengths, and we compare them with previous calculations in the literature. The new model enables extraction of rotational temperature, column abundance, and production rate from astronomical observations of CN in the inner coma of comets. Our model accounts for excitation and de-excitation of rotational levels in the ground vibrational state by collisions, solar excitation to the

and

electronically excited states followed by cascade to ro-vibrational levels of

, and direct solar infrared pumping of ro-vibrational levels in the

state. The model uses advanced solar spectra acquired at high spectral resolution at the relevant infrared and optical wavelengths and considers the heliocentric radial velocity of the comet (the Swings effect) when assessing the exciting solar flux for a given transition. We present model predictions for the variation of fluorescence rates with rotational temperature and heliocentric radial velocity. Furthermore, we test our fluorescence model by comparing predicted and measured line-by-line intensities for

(1–0) in comet C/2014 Q2 (Lovejoy), thereby identifying multiple emission lines observed at IR wavelengths.
A COMPARISON OF STELLAR ELEMENTAL ABUNDANCE TECHNIQUES AND MEASUREMENTS
Authors: Hinkel Natalie R. , Young Patrick A. , Pagano Michael D. , Desch Steven J. , Anbar Ariel D. , Adibekyan Vardan , Blanco-Cuaresma Sergi , Carlberg Joleen K. , Mena Elisa Delgado , Liu Fan , Nordlander Thomas , Sousa Sergio G. , Korn Andreas , Gruyters Pieter , Heiter Ulrike , Jofré Paula , Santos Nuno C. , Soubiran Caroline 
Published: August 2016

ABSTRACT
Stellar elemental abundances are important for understanding the fundamental properties of a star or stellar group, such as age and evolutionary history, as well as the composition of an orbiting planet. However, as abundance measurement techniques have progressed, there has been little standardization between individual methods and their comparisons. As a result, different stellar abundance procedures determine measurements that vary beyond the quoted error for the same elements within the same stars. The purpose of this paper is to better understand the systematic variations between methods and offer recommendations for producing more accurate results in the future. We invited a number of participants from around the world (Australia, Portugal, Sweden, Switzerland, and the United States) to calculate 10 element abundances (C, O, Na, Mg, Al, Si, Fe, Ni, Ba, and Eu) using the same stellar spectra for four stars (HD 361, HD 10700, HD 121504, and HD 202206). Each group produced measurements for each star using (1) their own autonomous techniques, (2) standardized stellar parameters, (3) a standardized line list, and (4) both standardized parameters and a line list. We present the resulting stellar parameters, absolute abundances, and a metric of data similarity that quantifies the homogeneity of the data. We conclude that standardization of some kind, particularly stellar parameters, improves the consistency between methods. However, because results did not converge as more free parameters were standardized, it is clear there are inherent issues within the techniques that need to be reconciled. Therefore, we encourage more conversation and transparency within the community such that stellar abundance determinations can be reproducible as well as accurate and precise.
Detection of Mycobacterium avium subsp. paratuberculosis in Iranian patients with type 1 diabetes mellitus by PCR and ELISA
Authors: Hesam Shariati Sonia , Alaei Anoosha , Keshavarz Rouhollah , Mosavari Nader , Rabbani Ali , Niegowska Magdalena , Sechi Leonardo A , Feizabadi Mohammad Mehdi 
Published: August 2016

Introduction: Mycobacterium avium subsp. paratuberculosis (MAP) is the causative agent of paratuberculosis or Johne’s disease in ruminants. Its role in triggering autoimmunity, including type 1 diabetes mellitus (T1DM), has been reported in recent years. Due to the high contamination rate of MAP in Iran’s livestock and the increasing outbreak of T1DM, we investigated this association in a small group of patients with T1DM in Iran. Methodology: Blood samples of 29 T1DM patients and 29 healthy control subjects were tested through enzyme-linked immunosorbent assay (ELISA) to detect antibodies against MAP3865c and ZnT8 homologous epitopes and the presence of MAP DNA. Blood samples were also cultured in mycobacterial growth indicator tubes and Herrold's egg yolk medium containing mycobactin J. Results: The results of ELISA showed a significant difference between T1DM patients and healthy group. IS900 was also detected in 51.72% of T1DM patients but in none of the control group. None of the samples grew in culture media. Conclusions: Due to the presence of MAP DNA and antibodies against MAP peptides in a significant number of T1DM patients compared with healthy control subjects, we may consider MAP as a possible trigger of T1DM in Iran. This indicates that exposure to MAP occurred in the positive subjects. Identifying the sources of contamination and routes of MAP transmission to humans seems necessary to prevent and reduce the burden of MAP infection in Iran.
Aesthetics, mysticism and the art of living
Authors: De Villiers Pieter G.R. 
Published: August 2016

This article analyses aesthetics and mysticism in the writings of Albert Geyser, the prominent South African theologian who is mostly known for his brave, uncompromising struggle against the apartheid system. In the first part of the article, brief introductory comments are made about Geyser’s theological and political role in South Africa in the light of his Protestan tcontext and his opposition to apartheid. It is then investigated how his reputation as a Biblical scholar and his protracted, much publicised stance against apartheid obfuscate his remarkable interest in aesthetics and mysticism and explains why his other theological interests and especially his interest in mysticism have not yet been researched. In the second part of the paper Geyser’s mystical interests are investigated by analysing his comments on church architecture, worship, music, liturgy and his pioneering translation of Thomas á Kempis’ Imitatio Christi.
A Simple Method for Computing Singular or Nearly Singular Integrals on Closed Surfaces
Authors: Beale J. Thomas , Ying Wenjun , Wilson Jason R. 
Published: August 2016

AbstractWe present a simple, accurate method for computing singular or nearly singular integrals on a smooth, closed surface, such as layer potentials for harmonic functions evaluated at points on or near the surface. The integral is computed with a regularized kernel and corrections are added for regularization and discretization, which are found from analysis near the singular point. The surface integrals are computed from a new quadrature rule using surface points which project onto grid points in coordinate planes. The method does not require coordinate charts on the surface or special treatment of the singularity other than the corrections. The accuracy is about O(h3), where h is the spacing in the background grid, uniformly with respect to the point of evaluation, on or near the surface. Improved accuracy is obtained for points on the surface. The treecode of Duan and Krasny for Ewald summation is used to perform sums. Numerical examples are presented with a variety of surfaces.
A Contact Line Dynamic Model for a Conducting Water Drop on an Electrowetting Device
Authors: He Dongdong , Huang Huaxiong 
Published: August 2016

AbstractThe static shape of drop under electrowetting actuation is well studied and recent electrowetting theory and experiments confirm that the local contact angle (microscopic angle) is unaffected while the apparent contact angle (macroscopic angle) is characterized by the Lippmann-Young equation. On the other hand, the evolution of the drop motion under electrowetting actuation has received less attention. In this paper, we investigate the motion of a conducting water drop on an electrowetting device (EWD) using the level set method. We derive a contact line two-phase flow model under electrowetting actuation using energy dissipation by generalizing an existing contact line model without the electric field. Our model is consistent with the static electrowetting theory as the dynamic contact angle satisfies the static Young's equation under equilibrium conditions. Our steady state results show that the apparent contact angle predicted by our model satisfies the Lippmann-Young's relation. Our numerical results based on the drop maximum deformation agree with experimental observations and static electrowetting theory. Finally, we show that for drop motion our results are not as good due to the difficulty of computing singular electric field accurately. Nonetheless, they provide useful insights and ameaningful first step towards the understanding of the drop dynamics under electrowetting actuation.
Efficient Semi-Lagrangian Vlasov-Maxwell Simulations of High Order Harmonic Generation from Relativistic Laser-Plasma Interactions
Authors: Lehmann Götz 
Published: August 2016

AbstractWe describe a relativistic semi-Lagrangian scheme for the numerical solution of the relativistic Vlasov-Maxwell system. The implementation strategy on a modern non-unified memory access (NUMA) architecture using the OpenMP framework is discussed. We demonstrated that close to perfect scaling can be obtained on modern many-core, multi-socket systems. Application of this code to the problem of relativistic generation of high-harmonic laser radiation is demonstrated. The results are compared to particle-in-cell (PIC) simulations, indicating in particular that for warm plasma the Vlasov simulation is superior. We discuss the impact of plasma temperature on the radiation spectrum and show that the efficiency of harmonic generation depends on the plasma temperature.