bluuebunny/crossref_metadata_2025_split huggingface dataset:
Deficits in Regional Cerebral Blood Flow on Brain SPECT Predict Treatment Resistant Depression
Authors: Amen Daniel G. , Taylor Derek V. , Meysami Somayeh , Raji Cyrus A. 
Published: March 2018

Background: Depression remains an important risk factor for Alzheimer’s disease, yet few neuroimaging biomarkers are available to identify treatment response in depression. Objective: To analyze and compare functional perfusion neuroimaging in persons with treatment resistant depression (TRD) compared to those experiencing full remission. Methods: A total of 951 subjects from a community psychiatry cohort were scanned with perfusion single photon emission computed tomography (SPECT) of the brain in both resting and task related settings. Of these, 78% experienced either full remission ( n = 506) or partial remission ( n = 237) and 11% were minimally responsive ( n = 103) or non-responsive (11%. n = 106). Severity of depression symptoms were used to define these groups with changes in the Beck Depression Inventory prior to and following treatment. Voxel-based analyses of brain SPECT images from full remission compared to the worsening group was conducted with the statistical parametric mapping software, version 8 (SPM 8). Multiple comparisons were accounted for with a false discovery rate ( p < 0.001). Results: Persons with depression that worsened following treatment had reduced cerebral perfusion compared to full remission in the multiple regions including the bilateral frontal lobes, right hippocampus, left precuneus, and cerebellar vermis. Such differences were observed on both resting and concentration SPECT scans. Conclusion: Our findings identify imaging-based biomarkers in persons with depression related to treatment response. These findings have implications in understanding both depression to prognosis and its role as a risk factor for dementia.
Surface Ice and Tholins on the Extreme Centaur 2012 DR30
Authors: Szabó Gy. M. , Kiss Cs. , Pinilla-Alonso N. , Hsiao E. Y. , Marion G. H. , Ries J. Györgyey , Duffard R. , Alvarez-Candal A. , Sárneczky K. , Vinkó J. 
Published: March 2018

Abstract
2012

is one of the known solar system objects with the largest aphelion distance, exceeding 2200 au, on a high inclination orbit (i = 78°). It has been recognized to be either a borderline representative of high inclination, high perihelion distance (HiHq) objects, or even a new class of bodies, similar to HiHq objects for orbit but with an aphelion in the inner Oort Cloud. Here, we present photometry using long-term data from 2000 to 2013 taken by the SDSS sky survey, ESO MPG 2.2 m and McDonald 2.1 m telescopes, and a visual+near-infrared spectrum taken with the Southern Astrophysical Research Telescope and Magellan telescopes, providing insights into the surface composition of this body. Our best fit suggests that the surface contains 60% of complex organics (30% of Titan and 30% of Triton tholins) with a significant fraction of ice (30%, including pure water and water with inclusions of complex organics) and 10% silicates. The models also suggest a low limit of amorphous carbons, and hence the fragmentation of long-chained complex organics is slower than their rate of generation. 2012

just recently passed the perihelion, and the long-term photometry of the object suggested ambiguous signs of activity, since the long-term photometric scatter well exceeded the supposed measurement errors and the expected brightness variation related to rotation. Photometric colors put 2012

exactly between dark neutral and red objects, thus it either can be in a transition phase between the two classes or have differing surface properties from these populated classes.
Simultaneous 13 cm/3 cm Single-pulse Observations of PSR B0329+54
Authors: Yan 闫 Zhen 振 , Shen 沈志 Zhi-Qiang 强 , Manchester R. N. , Ng C.-Y. , Weltevrede P. , Wang 王洪 Hong-Guang 光 , Wu 吴鑫 Xin-Ji 基 , Yuan 袁建 Jian-Ping 平 , Wu 吴亚 Ya-Jun 军 , Zhao 赵融 Rong-Bing 冰 , Liu 刘庆 Qing-Hui 会 , Zhao 赵汝 Ru-Shuang 双 , Liu 刘 Jie 杰 
Published: March 2018

Abstract
We have investigated the mode changing properties of PSR B0329+54 using 31 epochs of simultaneous 13 cm/3 cm single-pulse observations obtained with the Shanghai Tian Ma 65 m telescope. The pulsar was found in the abnormal emission mode 17 times, accounting for ∼13% of the 41.6 hr total observation time. Single-pulse analyses indicate that mode changes took place simultaneously at 13 cm/3 cm within a few rotational periods. We detected occasional bright and narrow pulses whose peak flux densities were 10 times higher than that of the integrated profile in both bands. At 3 cm, about 0.66% and 0.27% of single pulses were bright in the normal mode and abnormal mode, respectively, but at 13 cm the occurrence rate was only about 0.007%. We divided the pulsar radiation window into three components (C1, C2, and C3) corresponding to the main peaks of the integrated profile. The bright pulses preferentially occurred at pulse phases corresponding to the peaks of C2 and C3. Fluctuation spectra showed that C2 had excess red noise in the normal mode, but broad quasi-periodic features with central frequencies around 0.12 cycles/period in the abnormal mode. At 3 cm, C3 had a stronger quasi-periodic modulation centered around 0.06 cycles/period in the abnormal mode. Although there were some asymmetries in the two-dimensional fluctuation spectra, we found no clear evidence for systematic subpulse drifting. Consistent with previous low-frequency observations, we found a very low nulling probability for B0329+54, with upper limits of 0.13% and 1.68% at 13 cm/3 cm, respectively.
Kinematic Distances: A Monte Carlo Method
Authors: Wenger Trey V. , Balser Dana S. , Anderson L. D. , Bania T. M. 
Published: March 2018

Abstract
Distances to high-mass star-forming regions (HMSFRs) in the Milky Way are a crucial constraint on the structure of the Galaxy. Only kinematic distances are available for a majority of the HMSFRs in the Milky Way. Here, we compare the kinematic and parallax distances of 75 Galactic HMSFRs to assess the accuracy of kinematic distances. We derive the kinematic distances using three different methods: the traditional method using the Brand & Blitz rotation curve (Method A), the traditional method using the Reid et al. rotation curve and updated solar motion parameters (Method B), and a Monte Carlo technique (Method C). Methods B and C produce kinematic distances closest to the parallax distances, with median differences of 13% (0.43

) and 17% (0.42

), respectively. Except in the vicinity of the tangent point, the kinematic distance uncertainties derived by Method C are smaller than those of Methods A and B. In a large region of the Galaxy, the Method C kinematic distances constrain both the distances and the Galactocentric positions of HMSFRs more accurately than parallax distances. Beyond the tangent point along ℓ = 30°, for example, the Method C kinematic distance uncertainties reach a minimum of 10% of the parallax distance uncertainty at a distance of 14

. We develop a prescription for deriving and applying the Method C kinematic distances and distance uncertainties. The code to generate the Method C kinematic distances is publicly available and may be utilized through an online tool.
X-Ray Flare Oscillations Track Plasma Sloshing along Star-disk Magnetic Tubes in the Orion Star-forming Region
Authors: Reale Fabio , Lopez-Santiago Javier , Flaccomio Ettore , Petralia Antonino , Sciortino Salvatore 
Published: March 2018

Abstract
Pulsing X-ray emission tracks the plasma “echo” traveling in an extremely long magnetic tube that flares in an Orion pre-main sequence (PMS) star. On the Sun, flares last from minutes to a few hours and the longest-lasting ones typically involve arcades of closed magnetic tubes. Long-lasting X-ray flares are observed in PMS stars. Large-amplitude (∼20%), long-period (∼3 hr) pulsations are detected in the light curve of day-long flares observed by the Advanced CCD Imaging Spectrometer on-board Chandra from PMS stars in the Orion cluster. Detailed hydrodynamic modeling of two flares observed on V772 Ori and OW Ori shows that these pulsations may track the sloshing of plasma along a single long magnetic tube, triggered by a sufficiently short (∼1 hr) heat pulse. These magnetic tubes are ≥20 solar radii long, enough to connect the star with the surrounding disk.
The Role of Proton Cyclotron Resonance as a Dissipation Mechanism in Solar Wind Turbulence: A Statistical Study at Ion-kinetic Scales
Authors: Woodham Lloyd D. , Wicks Robert T. , Verscharen Daniel , Owen Christopher J. 
Published: March 2018

Abstract
We use magnetic field and ion moment data from the MFI and SWE instruments on board the Wind spacecraft to study the nature of solar wind turbulence at ion-kinetic scales. We analyze the spectral properties of magnetic field fluctuations between 0.1 and 5.4 Hz during 2012 using an automated routine, computing high-resolution 92 s power and magnetic helicity spectra. To ensure the spectral features are physical, we make the first in-flight measurement of the MFI “noise-floor” using tail-lobe crossings of the Earth’s magnetosphere during early 2004. We utilize Taylor’s hypothesis to Doppler-shift into the spacecraft frequency frame, finding that the spectral break observed at these frequencies is best associated with the proton cyclotron resonance scale, 1/k

c
, rather than the proton inertial length, d

i
, or proton gyroscale, ρ

i
. This agreement is strongest when we consider periods where

, and is consistent with a spectral break at d

i
for

and at ρ

i
for

. We also find that the coherent magnetic helicity signature observed at these frequencies is bounded at low frequencies by 1/k

c
, and its absolute value reaches a maximum at ρ

i
. These results hold in both slow and fast wind streams, but with a better correlation in the more Alfvénic fast wind where the helicity signature is strongest. We conclude that these findings are consistent with proton cyclotron resonance as an important mechanism for dissipation of turbulent energy in the solar wind, occurring at least half the time in our selected interval. However, we do not rule out additional mechanisms.
Unambiguous Evidence of Filament Splitting-induced Partial Eruptions
Authors: Cheng X. , Kliem B. , Ding M. D. 
Published: March 2018

Abstract
Coronal mass ejections are often considered to result from the full eruption of a magnetic flux rope (MFR). However, it is recognized that, in some events, the MFR may release only part of its flux, with the details of the implied splitting not completely established due to limitations in observations. Here, we investigate two partial eruption events including a confined and a successful one. Both partial eruptions are a consequence of the vertical splitting of a filament-hosting MFR involving internal reconnection. A loss of equilibrium in the rising part of the magnetic flux is suggested by the impulsive onset of both events and by the delayed onset of reconnection in the confined event. The remaining part of the flux might be line-tied to the photosphere in a bald patch (BP) separatrix surface, and we confirm the existence of extended BP sections for the successful eruption. The internal reconnection is signified by brightenings in the body of one filament and between the rising and remaining parts of both filaments. It evolves quickly into the standard current sheet reconnection in the wake of the eruption. As a result, regardless of being confined or successful, both eruptions produce hard X-ray sources and flare loops below the erupting but above the surviving flux, as well as a pair of flare ribbons enclosing the latter.
Transverse Wave Induced Kelvin–Helmholtz Rolls in Spicules
Authors: Antolin P. , Schmit D. , Pereira T. M. D. , De Pontieu B. , De Moortel I. 
Published: March 2018

Abstract
In addition to their jet-like dynamic behavior, spicules usually exhibit strong transverse speeds, multi-stranded structure, and heating from chromospheric to transition region temperatures. In this work we first analyze Hinode and IRIS observations of spicules and find different behaviors in terms of their Doppler velocity evolution and collective motion of their sub-structure. Some have a Doppler shift sign change that is rather fixed along the spicule axis, and lack coherence in the oscillatory motion of strand-like structure, matching rotation models, or long-wavelength torsional Alfvén waves. Others exhibit a Doppler shift sign change at maximum displacement and coherent motion of their strands, suggesting a collective magnetohydrodynamic (MHD) wave. By comparing with an idealized 3D MHD simulation combined with radiative transfer modeling, we analyze the role of transverse MHD waves and associated instabilities in spicule-like features. We find that transverse wave induced Kelvin–Helmholtz (TWIKH) rolls lead to coherence of strand-like structure in imaging and spectral maps, as seen in some observations. The rapid transverse dynamics and the density and temperature gradients at the spicule boundary lead to ring-shaped Mg ii k and Ca ii H source functions in the transverse cross-section, potentially allowing IRIS to capture the Kelvin–Helmholtz instability dynamics. Twists and currents propagate along the spicule at Alfvénic speeds, and the temperature variations within TWIKH rolls, produce the sudden appearance/disappearance of strands seen in Doppler velocity and in Ca ii H intensity. However, only a mild intensity increase in higher-temperature lines is obtained, suggesting there is an additional heating mechanism at work in spicules.
The Binary Neutron Star Event LIGO/Virgo GW170817 160 Days after Merger: Synchrotron Emission across the Electromagnetic Spectrum
Authors: Margutti R. , Alexander K. D. , Xie X. , Sironi L. , Metzger B. D. , Kathirgamaraju A. , Fong W. , Blanchard P. K. , Berger E. , MacFadyen A. , Giannios D. , Guidorzi C. , Hajela A. , Chornock R. , Cowperthwaite P. S. , Eftekhari T. , Nicholl M. , Villar V. A. , Williams P. K. G. , Zrake J. 
Published: March 2018

Abstract
We report deep Chandra X-ray Observatory (CXO), Hubble Space Telescope (HST), and Karl J. Jansky Very Large Array (VLA) observations of the binary neutron star event GW170817 at t < 160 days after merger. These observations show that GW170817 has been steadily brightening with time and might have now reached its peak, and constrain the emission process as non-thermal synchrotron emission where the cooling frequency ν

c
is above the X-ray band and the synchrotron frequency ν

m
is below the radio band. The very simple power-law spectrum extending for eight orders of magnitude in frequency enables the most precise measurement of the index p of the distribution of non-thermal relativistic electrons

accelerated by a shock launched by a neutron star (NS)–NS merger to date. We find p = 2.17 ± 0.01, which indicates that radiation from ejecta with Γ ∼ 3–10 dominates the observed emission. While constraining the nature of the emission process, these observations do not constrain the nature of the relativistic ejecta. We employ simulations of explosive outflows launched in NS ejecta clouds to show that the spectral and temporal evolution of the non-thermal emission from GW170817 is consistent with both emission from radially stratified quasi-spherical ejecta traveling at mildly relativistic speeds, and emission from off-axis collimated ejecta characterized by a narrow cone of ultra-relativistic material with slower wings extending to larger angles. In the latter scenario, GW170817 harbored a normal short gamma-ray burst (SGRB) directed away from our line of sight. Observations at t ≤ 200 days are unlikely to settle the debate, as in both scenarios the observed emission is effectively dominated by radiation from mildly relativistic material.
High-frequency Oscillations in the Atmosphere above a Sunspot Umbra
Authors: Wang Feng , Deng Hui , Li Bo , Feng Song , Bai Xianyong , Deng Linhua , Yang Yunfei , Xue Zhike , Wang Rui 
Published: March 2018

Abstract
We use high spatial and temporal resolution observations, simultaneously obtained with the New Vacuum Solar Telescope and Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory, to investigate the high-frequency oscillations above a sunspot umbra. A novel time–frequency analysis method, namely, the synchrosqueezing transform (SST), is employed to represent their power spectra and to reconstruct the high-frequency signals at different solar atmospheric layers. A validation study with synthetic signals demonstrates that SST is capable of resolving weak signals even when their strength is comparable to the high-frequency noise. The power spectra, obtained from both SST and the Fourier transform, of the entire umbral region indicate that there are significant enhancements between 10 and 14 mHz (labeled as 12 mHz) at different atmospheric layers. Analyzing the spectrum of a photospheric region far away from the umbra demonstrates that this 12 mHz component exists only inside the umbra. The animation based on the reconstructed 12 mHz component in AIA 171 Å illustrates that an intermittently propagating wave first emerges near the footpoints of coronal fan structures, and then propagates outward along the structures. A time–distance diagram, coupled with a subsonic wave speed (∼49 km s−1), highlights the fact that these coronal perturbations are best described as upwardly propagating magnetoacoustic slow waves. Thus, we first reveal the high-frequency oscillations with a period around one minute in imaging observations at different height above an umbra, and these oscillations seem to be related to the umbral perturbations in the photosphere.
L’évangile, promesse pour les pauvres
Authors: Odinet François 
Published: March 2018

Quand les personnes très pauvres méditent l’évangile, elles prennent Dieu au mot, en lisant l’Écriture comme une promesse, résonnant avec la promesse qui qualifie toute vie humaine. La rencontre de la promesse évangélique avec leur quotidien est de type pascal : elle peut faire surgir un cri qui révèle la puissance de leur prière, ou rendre compte de la résurrection. Elle peut encore attester la présence de Dieu là même où sa promesse paraît démentie. L’écho que les personnes très pauvres offrent à l’évangile se révèle ainsi plein d’une singulière autorité.
La contribution de la religion au projet politique de l’Europe
Authors: Dijon Xavier 
Published: March 2018

Le projet de construction européenne gagne-t-il à se référer à une confession religieuse ? Alors que les rationalistes récusent une telle liaison au nom de la laïcité, les croyants relisent l’histoire des grands mouvements qui ont parcouru l’Europe – paganisme et judaïsme, christianisme et islam, catholicisme et protestantisme, marxisme et nazisme – pour constater une remarquable convenance entre la tradition chrétienne et le projet européen lui-même.
Relationship Between Sensory Processing and Participation in Daily Occupations for Children With Autism Spectrum Disorder: A Systematic Review of Studies That Used Dunn’s Sensory Processing Framework
Authors: Ismael Noor , Lawson Lisa Mische , Hartwell Julie 
Published: March 2018

Abstract
Research measuring sensory processing in children with autism spectrum disorder (ASD) has shown variability in terms of measures used and participant ages, contributing to difficulty in interpreting and summarizing the findings of these studies. In an attempt to clarify the status of the literature, we conducted a systematic review of studies that focused on participation in daily occupations and evaluated sensory processing in children with ASD aged 5–13 yr using Dunn’s sensory processing framework. Evidence from 7 studies shows that sensory processing has a significant impact on participation in daily life of children with ASD. Included studies demonstrated medium and low levels of evidence. Additional research using more robust scientific methods is needed.
Nancy Meyers
Authors: Jermyn Deborah 
Published: March 2018

Nancy Meyers is acknowledged as the most commercially successful woman filmmaker of all time, described by Daphne Merkin in The New York Times on the release of It’s Complicated as ‘a singular figure in Hollywood – [she] may, in fact, be the most powerful female writer-director-producer currently working’. Yet Meyers remains a director who, alongside being widely dismissed by critics, has been largely absent in scholarly accounts both of contemporary Hollywood cinema, and of feminism and film. Despite Meyers’ impressive track record for turning a profit (including the biggest box-office return ever achieved by a woman filmmaker at that time for What Women Want in 2000), and a multifaceted career as a writer/producer/director dating back to her co-writing Private Benjamin in 1980, Meyers has been oddly neglected by Film Studies to date.
Including Nancy Meyers in the Bloomsbury Companions to Contemporary Filmmakers rectifies this omission, giving her the kind of detailed consideration and recognition she warrants and exploring how, notwithstanding the challenges authorship holds for feminist film studies, Meyers can be situated as a skilled ‘auteur’. This book proposes that Meyers’ box-office success, the consistency of style and theme across her films, and the breadth of her body of work as a writer/producer/director across more than three decades at the forefront of Hollywood (thus importantly bridging the second/third waves of feminism) make her a key contemporary US filmmaker. Structured to meet the needs of both the student and scholar, Jermyn's volume situates Meyers within this historical and critical context, exploring the distinctive qualities of her body of work, the reasons behind the pervasive resistance to it and new ways of understanding her films.