pinecone/core-2020-05-10-deduplication huggingface dataset:
Alfv\'en wave phase-mixing in flows: Why over-dense, solar coronal, open
  magnetic field structures are cool?

The motivation for this study is to include the effect of plasma flow in
Alfv\'en wave (AW) damping via phase mixing and to explore the observational
implications. Our magnetohydrodynamic (MHD) simulations and analytical
calculations show that, when a background flow is present, mathematical
expressions for the AW damping via phase mixing are modified by the following
substitution: $C_A^\prime(x) \to C_A^\prime(x)+V_0^\prime(x)$, where $C_A$ and
$V_0$ are AW phase and the flow speeds, and the prime denotes a derivative in
the direction across the background magnetic field. In uniform magnetic fields
and over-dense plasma structures, where $C_A$ is smaller than in the
surrounding plasma, the flow, which is confined to the structure and going in
the same direction as the AW, reduces the effect of phase-mixing, because on
the edges of the structure $C_A^\prime$ and $V_0^\prime$ have opposite signs.
Thus, the wave damps by means of slower phase-mixing compared to the case
without the flow. This is the result of the co-directional flow that reduces
the wave front stretching in the transverse direction. We apply our findings to
addressing the question why over-dense solar coronal open magnetic field
structures (OMFS) are cooler than the background plasma. Observations show that
the over-dense OMFS (e.g. solar coronal polar plumes) are cooler than
surrounding plasma and that, in these structures, Doppler line-broadening is
consistent with bulk plasma motions, such as AW. If over-dense solar coronal
OMFS are heated by AW damping via phase-mixing, we show that, co-directional
with AW, plasma flow in them reduces the phase-mixing induced-heating, thus
providing an explanation of why they appear cooler than the background.Comment: Accepted for publication in Astron. Astrophys. -- final accepted
  versio
The nature of LINER galaxies : ubiquitous hot old stars and rare accreting black holes

R.S. acknowledges support by the IMPRS for Astronomy & Cosmic Physics at the University of Heidelberg. K.J. is supported by the Emmy Noether-Programme of the German Science Foundation DFG under grant Ja 1114/3-2 and the German Space Agency DLR. G.v.d.V. and J.F.-B. acknowledge the DAGAL network from the People Programme (Marie Curie Actions) of the European Union’s Seventh Framework Programme FP7/2007-2013/ under REA grant agreement number PITN-GA-2011-289313. J.F.-B. further acknowledges financial support from the Ramón y Cajal Program and grant AYA2010-21322-C03-02 from the Spanish Ministry of Economy and Competitiveness (MINECO). V.W. acknowledges support from the ERC Starting Grant SEDmorph. R. A. Marino was also funded by the spanish programme of International Campus of Excellence Moncloa (CEI).Context. Galaxies, which often contain ionised gas, sometimes also exhibit a so-called low-ionisation nuclear emission line region (LINER). For 30 years, this was attributed to a central mass-accreting supermassive black hole (more commonly known as active galactic nucleus, AGN) of low luminosity, making LINER galaxies the largest AGN sub-population, which dominate in numbers over higher luminosity Seyfert galaxies and quasars. This, however, poses a serious problem. While the inferred energy balance is plausible, many LINERs clearly do not contain any other independent signatures of an AGN. Aims. Using integral field spectroscopic data from the CALIFA survey, we compare the observed radial surface brightness profiles with what is expected from illumination by an AGN. Methods. Essential for this analysis is a proper extraction of emission lines, especially weak lines, such as Balmer Hβ lines, which are superposed on an absorption trough. To accomplish this, we use the GANDALF code, which simultaneously fits the underlying stellar continuum and emission lines. Results. For 48 galaxies with LINER-like emission, we show that the radial emission-line surface brightness profiles are inconsistent with ionisation by a central point-source and hence cannot be due to an AGN alone. Conclusions. The most probable explanation for the excess LINER-like emission is ionisation by evolved stars during the short but very hot and energetic phase known as post-AGB. This leads us to an entirely new interpretation. Post-AGB stars are ubiquitous and their ionising effect should be potentially observable in every galaxy with the gas present and with stars older than ~1 Gyr unless a stronger radiation field from young hot stars or an AGN outshines them. This means that galaxies with LINER-like emission are not a class defined by a property but rather by the absence of a property. It also explains why LINER emission is observed mostly in massive galaxies with old stars and little star formation.Publisher PDFPeer reviewe
Variable stars in the globular cluster NGC 7492 : new discoveries and physical parameter determination

A.A.F. acknowledges financial support from DGAPA-UNAM grant through project IN104612. The authors are thankful to the CONACyT (México) and the Department of Science and Technology (India) for financial support under the Indo-Mexican collaborative project DST/INT/MEXICO/ RP001/2001.Aims. We have performed a photometric V,R,I CCD time-series analysis with a baseline of about eight years of the outer-halo globular cluster NGC 7492 with the aim of searching for new variables and using these (and the previously known variables) to determine the physical parameters of interest for the cluster (e.g. metallicity, absolute magnitude of the horizontal branch, distance, etc.). Methods. We used difference image analysis to extract precise light curves in the relatively crowded star field, especially towards the densely populated central region. Several different approaches were used for variability detection that recover the known variables and lead to new discoveries. We determined the physical parameters of the only RR0 star using a light-curve Fourier decomposition analysis. Results. We found one new long-period variable and two SX Phe stars in the blue straggler region. We also present one candidate SX Phe star that requires follow-up observations. Assuming that the SX Phe stars are cluster members and using the period-luminosity relation for these stars, we estimate their distances as ~25.2 ± 1.8 and 26.8 ± 1.8 kpc, and identify their possible modes of oscillation. We refined the periods of the two RR Lyrae stars in our field of view. We found that the RR1 star V2 is undergoing a period change and possibly exhibits the Blazhko effect. A Fourier decomposition of the light curve of the RR0 star V1 allowed us to estimate a metallicity of [Fe/H]ZW ~ −1.68 ± 0.10 or [Fe/H]UVES ~ −1.64 ± 0.13, a log-luminosity log (L/L⊙) ~ 1.76 ± 0.02, an absolute magnitude MV ~ 0.38 ± 0.04 mag, and a true distance modulus of μ0 ~ 16.93 ± 0.04 mag, which is equivalent to a distance of ~24.3 ± 0.5 kpc. All of these values are consistent with previous estimates in the literature.Publisher PDFPeer reviewe
Measurement of dijet production with a veto on additional central jet activity in pp collisions at ps = 7TeV using the ATLAS detector

A measurement of jet activity in the rapidity interval bounded by a dijet system
is presented. Events are vetoed if a jet with transverse momentum greater than 20GeV
is found between the two boundary jets. The fraction of dijet events that survive the jet
veto is presented for boundary jets that are separated by up to six units of rapidity and
with mean transverse momentum 50 < pT < 500GeV. The mean multiplicity of jets above
the veto scale in the rapidity interval bounded by the dijet system is also presented as an
alternative method for quantifying perturbative QCD emission. The data are compared to
a next-to-leading order plus parton shower prediction from the powheg-box, an all-order
resummation using the hej calculation and the pythia, herwig++ and alpgen event
generators. The measurement was performed using pp collisions at ps = 7TeV using data
recorded by the ATLAS detector in 2010
From bad to worse: Symbolic equivalence and opposition in fear generalization

The present study compared the impact of symbolic equivalence and opposition relations on fear generalization. In a procedure using nonsense words, some stimuli became symbolically equivalent to an aversively conditioned stimulus while others were symbolically opposite.
The generalization of fear to equivalently and oppositely related stimuli was then measured using behavioural avoidance, retrospective US expectancy and stimulus valence ratings.
Equivalence relations facilitated fear generalization while opposition relations constrained generalization. The potential clinical implications of symbolic generalization discussed.status: publishe
Neutrino mass generation and singly charged leptonic exotics in WW events

Current measurement of leptonic WW is significantly higher than the standard model prediction which may accommodate new physics signal that mimics the leptonic decaying W . We investigate a TeV neutrino mass generation model that predicts singly charged leptonic exotics. The collider signature of this model may mimic the leptonic WW search and evade all other searches. With introduction of new SU(2)L doublet leptons, singly charged exotic leptons L± decay into L±→ℓ±ϕ where ϕ is a light singlet scalar of O(MeV) that decays into neutrinos. Drell–Yan production of L+L−→ℓ+ℓ−+E̸T fits leptonic WW searches and L±L0→ℓ±+E̸T is completely buried in SM background. In the case of direct lepton from L -decay instead of secondary decay from leptonic τ±  we find the lower mass bound as 125 GeV of such exotic leptons that can be accommodated by the current measurements of WW searches at the LHC. To derive the upper bound, we employ both heavy Higgs boson search of di-lepton plus E̸T final state and leptonic W′ search of single lepton plus E̸T . Even though heavy Higgs is excluded between 260 and 640 GeV, we find LHC data can still accommodate L between 150 and 300 GeV after giving up the ηℓℓ cut. Using the single W′ search bound, we can obtain an approximate upper bound as 300 GeV
Causality & holographic entanglement entropy

We identify conditions for the entanglement entropy as a function of spatial region to be compatible with causality in an arbitrary relativistic quantum field theory. We then prove that the covariant holographic entanglement entropy prescription (which relates entanglement entropy of a given spatial region on the boundary to the area of a certain extremal surface in the bulk) obeys these conditions, as long as the bulk obeys the null energy condition. While necessary for the validity of the prescription, this consistency requirement is quite nontrivial from the bulk standpoint, and therefore provides important additional evidence for the prescription. In the process, we introduce a codimension-zero bulk region, named the entanglement wedge, naturally associated with the given boundary spatial region. We propose that the entanglement wedge is the most natural bulk region corresponding to the boundary reduced density matrix
Holographic entanglement entropy in 2D holographic superconductor via AdS3/CFT2

The aim of the present letter is to find the holographic entanglement entropy (HEE) in 2D holographic superconductors (HSC). Indeed, it is possible to compute the exact form of this entropy due to an advantage of approximate solutions inside normal and superconducting phases with backreactions. By making the UV and IR limits applied to the integrals, an approximate expression for HEE is obtained. In case the software cannot calculate minimal surface integrals analytically, it offers the possibility to proceed with a numerical evaluation of the corresponding terms. We'll understand how the area formula incorporates the structure of the domain wall approximation. We see that HEE changes linearly with belt angle. It's due to the extensivity of this type of entropy and the emergent of an entropic force. We find that the wider belt angle corresponds to a larger holographic surface. Another remarkable observation is that no “confinement/deconfinement” phase transition point exists in our 2D dual field theory. Furthermore, we observe that the slope of the HEE with respect to the temperature dSdT decreases, thanks to the emergence extra degree of freedom(s) in low temperature system. A first order phase transition is detected near the critical point
Contributions to the width difference in the neutral D system from hadronic decays

Recent studies of several multi-body D0 meson decays have revealed that the final states are dominantly CP -even. However, the small value of the width difference between the two physical eigenstates of the D0 – D‾0 system indicates that the total widths of decays to CP -even and CP -odd final states should be the same to within about a percent. The known contributions to the width difference from hadronic D0 decays are discussed, and it is shown that an apparent excess of quasi- CP -even modes is balanced, within current uncertainty, by interference effects in quasi-flavour-specific decays. Decay modes which may significantly affect the picture with improved measurements are considered
The media's role in intelligence democratization

The article of record as published may be found at http://dx.doi.org/10.1080/08850607.2014.842806In their path toward democratic consolidation, emerging democracies endeavor to ensure the democratic transfer of political power, bring changes in the legal framework, transform their executive, legislative, and
judicial systems, boost free market economy, and develop robust and functional civil societies. They also institutionalize democratic civil–military relations (CMR) by establishing new security institutions—military, police, and intelligence agencies—that are under democratic civilian control, effective, and efficient. Of these many tasks, the democratization of intelligence agencies is by far the most daunting, as effectiveness and
efficiency involve secrecy, while democratic control implies transparency, openness, and accountability. Nevertheless, democratic reform of intelligence in new democracies, though difficult, is not impossible, if and
when civilians are interested and willing to ‘‘invest’’ in intelligence and intelligence reform. The contribution of external factors, such as media, civil society, international groups, and individuals involved in human
rights, may also be instrumental in achieving a balance between control and effectiveness of intelligence
Moral disengagement, the dark triad, and unethical consumer attitudes

Purpose. Bandura's theory of moral disengagement explains how otherwise ethical persons\ud
can behave immorally. We examined whether a trait model of general personality and the "dark triad"\ud
underlay moral disengagement, the relationship these constructs have to unethical consumer attitudes,\ud
and whether moral disengagement provided incremental validity in the prediction of antisocial\ud
behaviour. Methods. Self-report data were obtained from a community sample of 380 adults via an online\ud
survey that administered all measures. Results. Correlations between unethical consumer\ud
attitudes, lower Agreeableness, lower Conscientiousness, higher moral disengagement, higher\ud
psychopathy, and higher Machiavellianism were captured by a single factor. When this broad factor\ud
was examined using regression, demographic, personality and the dark triad traits all predicted moral\ud
disengagement, specific influences being age, education, Intellect, psychopathy, and Machiavellianism.\ud
A similar model examining predictors of unethical consumer attitudes again found all blocks\ud
contributed to the outcome, with specific influence provided by age, Intellect, and moral\ud
disengagement, the latter showing incremental validity as a predictor of unethical consumer\ud
attitudes.Conclusions. Moral disengagement is based on low Agreeableness, Machiavellianism and\ud
psychopathic-type traits, but provides incremental validity in predicting antisocial attitudes to a trait\ud
model alone. Narcissism is neither related to moral disengagement, nor unethical consumer attitudes.Peer-reviewedPost-prin
A developmental approach to robotic pointing via human-robot interaction

This is an open access article under the CC\ud
BY license (http://creativecommons.org/licenses/by/3.0/)The ability of pointing is recognised as an essential skill of a robot in its communication and social interaction. This paper introduces a developmental learning approach to robotic pointing, by exploiting the interactions between a human and a robot. The approach is inspired through observing the process of human infant development. It works by first applying a reinforcement learning algorithm to guide the robot to create attempt movements towards a salient object that is out of the robot's initial reachable space. Through such movements, a human demonstrator is able to understand the robot desires to touch the target and consequently, to assist the robot to eventually reach the object successfully. The human-robot interaction helps establish the understanding of pointing gestures in the perception of both the human and the robot. From this, the robot can collect the successful pointing gestures in an effort to learn how to interact with humans. Developmental constraints are utilised to drive the entire learning procedure. The work is supported by experimental evaluation, demonstrating that the proposed approach can lead the robot to gradually gain the desirable pointing ability. It also allows that the resulting robot system exhibits similar developmental progress and features as with human infants
Determinants of changes in sedentary time and breaks in sedentary time among 9 and 12 year old children

The current study aimed to identify the determinants of objectively measured changes in sedentary time and sedentary fragmentation from age 9 - to age 12 years. Data were collected as part of the Gateshead Millennium Birth Cohort study from September 2008 - August 2009 and from January 2012 - November 2012. Participants were 9.3 (±0.4) years at baseline (n=508) and 12.5 (±0.3) years at follow-up (n=427). Sedentary behaviour was measured using an ActiGraph GT1M accelerometer. Twenty potential determinants were measured, within a socio-ecological model, and tested for their association with changes in sedentary time and the extent to which sedentary behaviour is prolonged or interrupted (fragmentation index). Univariate and multivariate linear regression analysis were conducted. Measurements taken during winter and a greater decrease in moderate-to-vigorous intensity physical activity (MVPA) over time were associated with larger increases in sedentary time (seasonality β:-3.03; 95% CI:-4.52,-1.54; and change in MVPA β:-1.68; 95% CI:-1.94, -1.41). Attendance at sport clubs was associated with smaller increases in sedentary time (-1.99; -3.44, -0.54). Girls showed larger decreases in fragmentation index (-0.52; -1.01, -0.02). Interventions aimed at decreasing the decline in MVPA and increasing/maintaining sport club attendance may prevent the rise in sedentary time as children grow older. In addition, winter could be targeted to prevent an increase in sedentary time and reduction in sedentary fragmentation during this season
Tracing jet emission at the base of a high-mass YSO. First AMBER/VLTI
  observations of the Br\gamma emission in IRAS 13481-6124

To probe the circumstellar environment of IRAS 13481-6124, a 20 M_sun
high-mass young stellar object (HMYSO) with a parsec-scale jet and accretion
disc, we investigate the origin of its Br\gamma-emission line through NIR
interferometry. We present the first AMBER/VLTI observations of the
Br\gamma-emitting region in an HMYSO at R~1500. Our AMBER/VLTI observations
reveal a spatially and spectrally resolved Br\gamma-line in emission with a
strong P Cygni profile, indicating outflowing matter with a terminal velocity
of ~500 km/s. Visibilities, differential phases, and closure phases are
detected in our observations within the spectral line and in the adjacent
continuum. Both total visibilities (continuum plus line emitting region) and
pure-line visibilities indicate that the Br\gamma-emitting region is more
compact (2-4 mas in diameter or ~6-13 au at 3.2 kpc) than the
continuum-emitting region (~5.4 mas or ~17 au). The absorption feature is also
spatially resolved at the longest baselines (81 and 85 m) and has a visibility
that is slightly smaller than the continuum-emitting region. The differential
phases at the four longest baselines display an \u2018S\u2019-shaped structure
across the line, peaking in the blue- and red-shifted high-velocity components.
The calibrated photocentre shifts are aligned with the known jet axis, i.e they
are probably tracing an ionised jet. The high-velocity components (v_r~100-500
km/s) are located far from the source, whereas the low-velocity components
(0-100 km/s) are observed to be closer, indicating a strong acceleration of the
gas flow in the inner 10 au. Finally, a non-zero closure phase along the
continuum is detected. By comparing our observations with the synthetic images
of the continuum around 2.16 um, we confirm that this feature originates from
the asymmetric brightness distribution of the continuum owing to the
inclination of the inner disc.Comment: To be published in A&A letter
3D electron density distribution in the solar corona during solar minima: assessment for more realistic solar wind modelling

PublishedArticle© 2015. The American Astronomical Society. All rights reserved. Article published in The Astrophysical Journal, Volume 814, Number 1Knowledge of the electron density distribution in the solar corona put constraints on the magnetic field configurations for coronal modeling and on initial conditions for solar wind modeling. We work with polarized SOHO/LASCO-C2 images from the last two recent minima of solar activity (1996–1997 and 2008–2010), devoid of coronal mass ejections. The goals are to derive the 4D electron density distributions in the corona by applying a newly developed time-dependent tomographic reconstruction method and to compare the results between the two solar minima and with two magnetohydrodynamic models. First, we confirm that the values of the density distribution in thermodynamic models are more realistic than in polytropic ones. The tomography provides more accurate distributions in the polar regions, and we find that the density in tomographic and thermodynamic solutions varies with the solar cycle in both polar and equatorial regions. Second, we find that the highest-density structures do not always correspond to the predicted large-scale heliospheric current sheet or its helmet streamer but can follow the locations of pseudo-streamers. We deduce that tomography offers reliable density distributions in the corona, reproducing the slow time evolution of coronal structures, without prior knowledge of the coronal magnetic field over a full rotation. Finally, we suggest that the highest-density structures show a differential rotation well above the surface depending on how they are magnetically connected to the surface. Such valuable information on the rotation of large-scale structures could help to connect the sources of the solar wind to their in situ counterparts in future missions such as Solar Orbiter and Solar Probe Plus