pinecone/core-2020-05-10-deduplication huggingface dataset:
Development of residual stress in sol-gel derived Pb(Zr,Ti)O3 films: An experimental study

Residual stresses develop in the sol-gel-derived ferroelectric thin films during the transformation of the metalorganic gel to the metal oxide upon thermal treatment and due to the thermal and elastic mismatch between the Pb(Zrx,Ti1-x)O3 (PZT) film and the substrate materials during cooling. In this study, residual stresses were determined using the wafer curvature method after the deposition of multilayer PZT film on platinized (100) silicon wafers. A multilayer model for stress analysis was used to calculate the residual stress in PZT films of three different compositions, x=0.4, x=0.52 and x=0.6. Orientation dependent residual stresses were found in compositions containing the tetragonal phase, with x=0.4 and x=0.52. Depending on the fraction of (100) orientated domains low compressive or low tensile stress was found in Pb(Zr0.4Ti0.6)O3 (PZT 40/60). Higher residual stress was found in PZT films consisting of only rhombohedral crystallographic structure (PZT 60/40) while the residual stress in PZT films with morphotropic boundary composition (PZT 52/48) was significantly dependent on the film orientation and the phase composition and could range from 17 MPa to 90 MPa. The effect of the film orientation on residual stress was found to be a function of the anisotropic thermal expansion coefficient of PZT. The contribution of the thermal and elastic properties of materials to the total wafer curvature was investigated and discussed. Finally, the residual stress results calculated with the four layers model were compared to the results calculated using the Stoney equation
The influence of meteorological variables on CO2 and CH4 trends recorded at a semi-natural station

CO2 and CH4 evolution is usually linked with sources, sinks and their changes. However, this study highlights the role of meteorological variables. It aims to quantify their contribution to the trend of these greenhouse gases and to determine which contribute most. Six years of measurements at a semi-natural site in northern Spain were considered. Three sections are established: the first focuses on monthly deciles, the second explores the relationship between pairs of meteorological variables, and the third investigates the relationship between meteorological variables and changes in CO2 and CH4. In the first section, monthly outliers were more marked for CO2 than for CH4. The evolution of monthly deciles was fitted to three simple expressions, linear, quadratic and exponential. The linear and exponential are similar, whereas the quadratic evolution is the most flexible since it provided a variable rate of concentration change and a better fit. With this last evolution, a decrease in the change rate was observed for low CO2 deciles, whereas an increasing change rate prevailed for the rest and was more accentuated for CH4. In the second section, meteorological variables were provided by a trajectory model. Backward trajectories from 1-day prior to reaching the measurement site were used to calculate distance and direction averages as well as the recirculation factor. Terciles of these variables were determined in order to establish three intervals with low, medium and high values. These intervals were used to classify the
variables following their interval widths and skewnesses. The best correlation between pairs of meteorological variables was observed for the average distance, in particular with horizontal wind speed. Sinusoidal relationships with the average direction were obtained for average distance and for vertical wind speed. Finally, in the third section, the quadratic evolution was considered in each interval of all the meteorological variables. As regards the main result, the greatest increases were obtained for high potential temperature for both gases followed by low and medium boundary layer height for CO2 and CH4, respectively. Combining both meteorological variables provided increases of 22 ± 9 and 0.070 ± 0.019 ppm for CO2 and CH4, respectively, although the number of observations affected is small, around 7%.Ministry of Economy and Competitiveness and ERDF funds (project numbers CGL2009-11979 and CGL2014-53948-P
Form follows function: pragmatic controlled trials (PCTs) have to answer different questions and require different designs than randomized controlled trials (RCTs).

Aim Rising concern for demonstrated real world comparative
effectiveness has heightened interest in “pragmatic trials”
design. Pragmatic trials investigate whether the efficacy, presumed
or found in explanatory trials under ideal conditions,
can also be detected under real world conditions, i.e. effectiveness.
It is also recognized that ‘real world’ effects which
are usually addressed in public health research gain growing
interest in confirming the ‘road capability’ of results obtained
under ideal study conditions. This paper demonstrates that
studies under ideal or real world conditions use different
methods, generate different information and cannot replace
each other.
Subjects and methods The PCT design meets four requirements
of public health and of effectiveness research. It
includes all individuals who presented with the selected
condition. It classifies the included individuals according
to baseline risks. It enables plausibility controls. Finally, it
compares the outcomes resulting from specified and notspecified
interventions or treatments.
Proposal We propose a pragmatic controlled trial (PCT)
design in which patient preference and other co-factors
crucial in determining the actual effectiveness of interventional
options will not be neutralized by concealed randomization
and blinding. This design is applicable to record the
selected interventions and generated outcomes in day-to-day
health care and is capable of incorporating preference and
other participative factors into assessment of effectiveness.
Conclusions The PCT design is useful for public health research,
e.g. the effectiveness of interventions to change smoking
habits or to prevent death frombreast cancer, as well as for
comparative effectiveness research where it will supplement
the traditional randomized controlled trial (RCT)
Severe disruption of the cytoskeleton and immunologically relevant surface molecules in a human macrophageal cell line in microgravity — Results of an in vitro experiment on board of the Shenzhou-8 space mission

During spaceflight the immune system is one of the most affected systems of the human body. During the SIMBOX (Science in Microgravity Box) mission on Shenzhou-8, we investigated microgravity-associated long-term alterations in macrophageal cells, the most important effector cells of the immune system. We analyzed the effect of long-term microgravity on the cytoskeleton and immunologically relevant surface molecules. Human U937 cells were differentiated into a macrophageal phenotype and exposed to microgravity or 1g on a reference centrifuge on-orbit for 5 days. After on-orbit fixation, the samples were analyzed with immunocytochemical staining and confocal microscopy after landing. The unmanned Shenzhou-8 spacecraft was launched on board a Long March 2F (CZ-2F) rocket from the Jiuquan Satellite Launch Center (JSLC) and landed after a 17-day-mission. We found a severely disturbed actin cytoskeleton, disorganized tubulin and distinctly reduced expression of CD18, CD36 and MHC-II after the 5 days in microgravity. The disturbed cytoskeleton, the loss of surface receptors for bacteria recognition, the activation of T lymphocytes, the loss of an important scavenger receptor and of antigen-presenting molecules could represent a dysfunctional macrophage phenotype. This phenotype in microgravity would be not capable of migrating or recognizing and attacking pathogens, and it would no longer activate the specific immune system, which could be investigated in functional assays. Obviously, the results have to be interpreted with caution as the model system has some limitations and due to numerous technical and biological restrictions (e.g. 23 °C and no CO2 supply during in-flight incubation). All parameter were carefully pre-tested on ground. Therefore, the experiment could be adapted to the experimental conditions available on Shenzhou-8
Longitudinal scaling property of the charge balance function in Au + Au
  collisions at 200 GeV

We present measurements of the charge balance function, from the charged
particles, for diverse pseudorapidity and transverse momentum ranges in Au + Au
collisions at 200 GeV using the STAR detector at RHIC. We observe that the
balance function is boost-invariant within the pseudorapidity coverage [-1.3,
1.3]. The balance function properly scaled by the width of the observed
pseudorapidity window does not depend on the position or size of the
pseudorapidity window. This scaling property also holds for particles in
different transverse momentum ranges. In addition, we find that the width of
the balance function decreases monotonically with increasing transverse
momentum for all centrality classes.Comment: 6 pages, 3 figure
The general behavior of $NLO$ unintegrated parton distributions based on
  the single-scale evolution and the angular ordering constraint

To overcome the complexity of generalized two hard scale ($k_t$,$\mu$)
evolution equation, well known as the $Ciafaloni$, $Catani$, $Fiorani$ and
$Marchsini$ ($CCFM$) evolution equations, and calculate the unintegrated parton
distribution functions ($UPDF$), $Kimber$, $Martin$ and $Ryskin$ ($KMR$)
proposed a procedure based on ($i$) the inclusion of single-scale ($\mu$) only
at the last step of evolution and ($ii$) the angular ordering constraint
($AOC$) on the $DGLAP$ terms (the $DGLAP$ collinear approximation), to bring
the second scale, $k_t$ into the $UPDF$ evolution equations. In this work we
intend to use the $MSTW 2008$ (Martin et al) parton distribution functions
(PDF) and try to calculate $UPDF$ for various values of $x$ (the longitudinal
fraction of parton momentum), $\mu$ (the probe scale) and $k_t$ (the parton
transverse momentum) to see the general behavior of three dimensional $UPDF$ at
the $NLO$ level up to the $LHC$ working energy scales ($\mu^2)$. It is shown
that there exits some pronounced peaks for the three dimensional $UPDF$
$(f_a(x,k_t))$ with respect to the two variables $x$ and $k_t$ at various
energies ($\mu$). These peaks get larger and move to larger values of $k_t$, as
the energy ($\mu$) is increased. We hope these peaks could be detected in the
$LHC$ experiments at $CERN$ and other laboratories in the less exclusive
processes
WASP-35b, WASP-48b and WASP-51b: Two new planets and an independent
  discovery of HAT-P-30b

We report the detection of WASP-35b, a planet transiting a metal-poor ([Fe/H]
= -0.15) star in the Southern hemisphere, WASP-48b, an inflated planet which
may have spun-up its slightly evolved host star of 1.75 R_sun in the Northern
hemisphere, and the independent discovery of HAT-P-30b / WASP-51b, a new planet
in the Northern hemisphere. Using WASP, RISE, FTS and TRAPPIST photometry, with
CORALIE, SOPHIE and NOT spectroscopy, we determine that WASP-35b has a mass of
0.72 +/- 0.06 M_J and radius of 1.32 +/- 0.03 R_J, and orbits with a period of
3.16 days, WASP-48b has a mass of 0.98 +/- 0.09 M_J, radius of 1.67 +/- 0.08
R_J and orbits in 2.14 days, while WASP-51b, with an orbital period of 2.81
days, is found to have a mass of 0.76 +/- 0.05 M_J and radius of 1.42 +/- 0.04
R_J, agreeing with values of 0.71 +/- 0.03 M_J and 1.34 +/- 0.07 R_J reported
for HAT-P-30b.Comment: 24 pages, 10 figures, submitted to A
Star cluster ecology IVa: Dissection of an open star
  cluster---photometry

The evolution of star clusters is studied using N-body simulations in which
the evolution of single stars and binaries are taken self-consistently into
account. Initial conditions are chosen to represent relatively young Galactic
open clusters, such as the Pleiades, Praesepe and the Hyades. The calculations
include a realistic mass function, primordial binaries and the external
potential of the parent Galaxy. Our model clusters are generally significantly
flattened in the Galactic tidal field, and dissolve before deep core collapse
occurs. The binary fraction decreases initially due to the destruction of soft
binaries, but increases later because lower mass single stars escape more
easily than the more massive binaries. At late times, the cluster core is quite
rich in giants and white dwarfs. There is no evidence for preferential
evaporation of old white dwarfs, on the contrary the formed white dwarfs are
likely to remain in the cluster. Stars tend to escape from the cluster through
the first and second Lagrange points, in the direction of and away from the
Galactic center. Mass segregation manifests itself in our models well within an
initial relaxation time. As expected, giants and white dwarfs are much more
strongly affected by mass segregation than main-sequence stars. Open clusters
are dynamically rather inactive. However, the combined effect of stellar mass
loss and evaporation of stars from the cluster potential drives its dissolution
on a much shorter timescale than if these effects are neglected. The often-used
argument that a star cluster is barely older than its relaxation time and
therefore cannot be dynamically evolved is clearly in error for the majority of
star clusters.Comment: reduced abstract, 33 pages (three separate color .jpg figures),
  submitted to MNRA
On the variational principle for dust shells in General Relativity

The variational principle for a thin dust shell in General Relativity is
constructed. The principle is compatible with the boundary-value problem of the
corresponding Euler-Lagrange equations, and leads to ``natural boundary
conditions'' on the shell. These conditions and the gravitational field
equations which follow from an initial variational principle, are used for
elimination of the gravitational degrees of freedom. The transformation of the
variational formula for spherically-symmetric systems leads to two natural
variants of the effective action. One of these variants describes the shell
from a stationary interior observer's point of view, another from the exterior
one. The conditions of isometry of the exterior and interior faces of the shell
lead to the momentum and Hamiltonian constraints. The canonical equivalence of
the mentioned systems is shown in the extended phase space. Some particular
cases are considered.Comment: 25 pages, RevTeX, no figures, revised version, typos corrected,
  accepted for publication in Journal of Mathematical Physic
The long bar as seen by the VVV survey: I. Colour-magnitude diagrams

The VISTA Variable Survey (VVV) is able to map the Galaxy at l<0 with an
unpaired depth (at least 3 mag deeper than 2MASS), opening new possibilities
for studying the inner structure of the Milky Way. In this paper we concentrate
on the exploitation of these data to better understand the spatial disposition
and distribution of the structures present in the inner Milky Way, particularly
the Long Bar and its interaction with the inner disc.
  The observations show the presence of a clear overdensity of stars with
associated recent stellar formation that we interpret as the traces of the Long
Bar, and we derive an angle for it of 41+/-5 with the Sun-Galactic centre line,
touching the disc near l=27 and l=-12. The colour-magnitude diagrams presented
here also show a lack of disc stars in several lines of sight, a fact that we
associate with the truncation of the disc by the potential of this bar for
Galactocentric radius less than 5kpc.Comment: Accepted for publication on A&A. Minor typos correcte
NNLO QCD corrections to jet production at hadron colliders from gluon
  scattering

We present the next-to-next-to-leading order (NNLO) QCD corrections to dijet
production in the purely gluonic channel retaining the full dependence on the
number of colours. The sub-leading colour contribution in this channel first
appears at NNLO and, as expected, increases the NNLO correction by around 10%
and exhibits a pT dependence, rising from 8% at low pT to 15% at high pT . The
present calculation demonstrates the utility of the antenna subtraction method
for computing the full colour NNLO corrections to dijet production at the Large
Hadron Collider.Comment: 33 pages, 4 figure
Astrophysical parameters of the peculiar X-ray transient IGR J11215-5952

The hard X-ray source IGR J11215-5952 is a peculiar transient, displaying
very short X-ray outbursts every 165 days. We obtained high-resolution spectra
of the optical counterpart, HD 306414, at different epochs, spanning a total of
three months, before and around the 2007 February outburst with the combined
aims of deriving its astrophysical parameters and searching for orbital
modulation. We fit model atmospheres generated with the fastwind code to the
spectrum. We also cross-correlated each individual spectrum to the best-fit
model to derive radial velocities. From its spectral features, we classify HD
306414 as B0.5 Ia. From the model fit, we find Teff = 24 700 K and log g = 2.7,
in good agreement with the morphological classification. Using the interstellar
lines in its spectrum, we estimate a distance to HD 306414 d > 7 kpc. Assuming
this distance, we derive R* = 40 Rsol and Mspect = 30 Msol (consistent, within
errors, with Mevol = 38 Msol). Radial velocity changes are not dominated by the
orbital motion, and we find an upper limit on the semi-amplitude for the
optical component Kopt < 11 +- 6 km/s. Large variations in the depth and shape
of photospheric lines suggest the presence of strong pulsations, which may be
the main cause of the radial velocity changes. Very significant variations,
uncorrelated with those of the photospheric lines are seen in the shape and
position of the Halpha emission feature around the time of the X-ray outburst,
but large excursions are also observed at other times. HD 306414 is a normal
B0.5 Ia supergiant. Its radial velocity curve is dominated by an effect that is
different from binary motion, and is most likely stellar pulsations. The data
available suggest that the X-ray outbursts are caused by the close passage of
the neutron star in a very eccentric orbit, perhaps leading to localised mass
outflow. (abridged).Comment: 10 pages, 9 figures, 4 table
Invisible Z' and dark matter: LHC vs LUX constraints

We consider a simple, yet generic scenario in which a new heavy $Z'$ gauge
boson couples both to SM fermions and to dark matter. In this framework we
confront the best LHC limits on an extra gauge boson $Z'$ to the constraints on
couplings to dark matter from direct detection experiments. In particular we
show that the LHC searches for resonant production of dileptons and the recent
exclusion limits obtained by the LUX collaboration give complementary
constraints. Together, they impose strong bounds on the invisible branching
ratio and exclude a large part of the parameter space for generic $Z'$ models.
Our study encompasses many possible $Z'$ models, including SSM, $E_6$-inspired
or B-L scenario.Comment: Figure and references added. Accepted for publication in JHE
The Infrared Structure of QCD Amplitudes and $H\to g g$ in FDH and DRED

We consider variants of dimensional regularization, including the
four-dimensional helicity scheme (FDH) and dimensional reduction (DRED), and
present the gluon and quark form factors in the FDH scheme at
next-to-next-to-leading order. We also discuss the generalization of the
infrared factorization formula to FDH and DRED. This allows us to extract the
cusp anomalous dimension as well as the quark and gluon anomalous dimensions at
next-to-next-to-leading order in the FDH and DRED scheme, using
$\overline{\text{MS}}$ and $\overline{\text{DR}}$ renormalization. To obtain
these results we also present the renormalization procedure in these schemes
Generalized string functions of N = 1 space-time supersymmetric string vacua

We present a dual formulation of the construction of N=2 nonlinear sigma-model type conformal field theories with c=9 which are mainly used as internal sectors of Calabi-Yau heterotic string compactifications. The supercurrents and the higher components of the spectral flow superfields turn out in each case to be tensor products of two simple currents of a c=1 and a non-supersymmetric parafermionic c=8 CFT. The characters of the latter model can be regarded as string functions of the coset sigma/U(1). In particular, for the (1)^9 Gepner model we discuss these string functions in detail, realizing this model contains a broken E_8 gauge symmetry of which only the abelian subalgebra remains a symmetry of the spectrum. As an example, we construct a simple model leading to a string theory with a massless spectrum of 36 E_6 generations and an extended gauge symmetry E_6 x SU(3)^4
Measurement of the Mass and Width of the W Boson in $e^{+}e^{-}$ Collisions at 189 GeV

The mass and width of the W boson are determined in e+e- collisions at LEP using 183 pb^-1 of data recorded at a centre-of-mass energy roots=189 GeV with the OPAL detector. The invariant mass distributions from 970 WW->qqqq and 1118 WW->qqln candidate events are used to measure the mass of the W boson, Mw = 80.451 +- 0.076(stat.) +- 0.049(syst.) GeV. A direct measurement of the width of the W boson gives Gw=2.09 +- 0.18(stat.) +- 0.09(syst.) GeV. The results are combined with previous OPAL results from 78 pb^-1 of data recorded with roots from 161 to 183 GeV, to obtain: Mw = 80.432 +- 0.066(stat.) +- 0.045(syst.) GeV, Gw = 2.04 +- 0.16(stat.) +- 0.09(syst.) GeV. The consistency of the direct measurement of Mw with that inferred from other measurements of electroweak parameters provides an important test of the Standard Model of electroweak interactions
Central charges, S-duality and massive vacua of N=1* super Yang-Mills

We provide a simple derivation of the extremal values of the superpotential
in massive vacua of N=1* SYM, making use of the required modular weight for the
central charge of BPS walls interpolating between these vacua. This modular
weight descends from the action of S-duality on the N=4 superalgebra which in
turn is inherited from its classical action on the dyon spectrum. We show that
this kinematic information, combined with minimal knowledge of the weak
coupling asymptotics, is sufficient to determine the exact vacuum
superpotentials in terms of Eisenstein series.Comment: 8 pages; v2: reference added, to appear in Phys. Lett.
The Sylvester-Gallai Theorem, colourings and algebra

Our point of departure is the following simple common generalisation of the
Sylvester-Gallai theorem and the Motzkin-Rabin theorem:
  Let S be a finite set of points in the plane, with each point coloured red or
blue or with both colours. Suppose that for any two distinct points A,B in S
sharing a colour there is a third point C in S, of the other colour, collinear
with A and B. Then all the points in S are collinear.
  We define a chromatic geometry to be a simple matroid for which each point is
coloured red or blue or with both colours, such that for any two distinct
points A,B in S sharing a colour there is a third point C in S, of the other
colour, collinear with A and B. This is a common generalisation of proper
finite linear spaces and properly two-coloured finite linear spaces, with many
known properties of both generalising as well. One such property is Kelly's
complex Sylvester-Gallai theorem. We also consider embeddings of chromatic
geometries in Desarguesian projective spaces. We prove a lower bound of 51 for
the number of points in a 3-dimensional chromatic geometry in projective space
over the quaternions. Finally, we suggest an elementary approach to the
corollary of an inequality of Hirzebruch used by Kelly in his proof of the
complex Sylvester-Gallai theorem.Comment: 23 pages, 3 figure