bluuebunny/crossref_metadata_2025_split huggingface dataset:
Usability of the Thera-Band® to improve foot drop in stroke survivors
Authors: Song SunHae , Park JungHee , Song GyuDong , Lee SeulGi , Jo YoHan , Jin MinKyung , Lee DongGeon , Jung SunHye , Hong SoungKyun , Lee SeungHoo , Pyo SeungHyeon , Lee GyuChang 
Published: April 2018

BACKGROUND: Stroke survivors show “foot drop”, dragging their toes on the ground in the swing phase of gait. Ineffective ankle dorsiflexion may result in an abnormal gait pattern. OBJECTIVE: The purpose of this study was to investigate the effect of ankle Thera-Band® use on gait patterns in stroke survivors. METHODS: Gait data were collected in eight subjects who had had strokes using gait analysis system, both with and without the Thera-Band®. The following dependent variables of gait parameters were analyzed: velocity, cadence, step length, stride length, single support time, and double support time. RESULTS: There were significant improvements in gait velocity, cadence, stride length, and double support time in those who used the Thera-Band® compared to those who did not ( p <  0.05). However, there were no significant differences in step length or single support time ( p >  0.05). CONCLUSIONS: The results show that ankle Thera-Band® use may have a positive effect in improving gait parameters by increasing the ankle stability in stroke survivors with foot drop. Its usefulness in the rehabilitation of foot drop in stroke survivors needs to be further investigated.
À propos des origines de la mosquée javanaise
Authors: Njoto Hélène 
Published: April 2018

La genèse du type dit de la « mosquée javanaise », à plan concentrique et à toits superposés, répandu à Java mais aussi dans le monde malais, est sujette à débat. Pour certains spécialistes, ce type aurait été importé de l'Inde, à l'époque islamisée, donc tardivement. Pour d'autres, il se serait développé à Java avant l'islamisation, puis aurait été adopté pour les besoins du nouveau culte musulman vers le XVe siècle. Dans la continuité d'une réflexion ébauchée par quelques historiens et architectes, cet article propose de faire le point sur cette dernière hypothèse, à la lumière de nouvelles sources archéologiques et d'une iconographie peu exploitée. Si ces sources montrent bien l'antériorité du type de bâtiments à toits superposés et plan concentrique répandu à la période hindo-bouddhique, elles permettent également de déterminer que ce type était bien en usage, pour les cultes hindouiste et bouddhiste, dès le VIIe siècle à Java Ouest, vers les VIIIe et IXe siècles à Java Centre et au Xe siècle au moins à Java Est.
Histoire d’un groupe de parenté du Fujian. Commerce au-delà des mers et mouvance
Authors: Salmon Claudine , Calanca Paola 
Published: April 2018

La découverte fortuite à Makassar d’une généalogie des Li originaires de Xiamen au Fujian nous incita à entreprendre une recherche dans l’île. Si la généalogie d’origine a disparu nous pûmes néanmoins retrouver le temple ancestral alors en reconstruction et divers membres du lignage. Cette rencontre allait donner lieu pour nous à deux recherches parallèles : l’une visant à retracer l’histoire des Li dans le temps long ; l’autre s’intéressant à la résurgence de ce groupe de parenté dans les années 2010. Quant aux Li de Xiamen, la lecture de leur généalogie les amena à entreprendre de leur côté une vaste enquête dans le temps et dans l’espace relative à leurs origines et à leur parentèle, les incitant à renouer avec des pratiques cultuelles et à ranimer leurs souvenirs. Cette quête familiale s’inscrit dans le grand mouvement de recherche des racines qui traverse tout le monde chinois. De plus, cet essai d’histoire prosopographique révèle, en arrière-plan, celle de la région dans son ensemble.
The KMTNet/K2-C9 (Kepler) Data Release
Authors: Kim H.-W. , Hwang K.-H. , Kim D.-J. , Albrow M. D. , Cha S.-M. , Chung S.-J. , Gould A. , Han C. , Jung Y. K. , Kim S.-L. , Lee C.-U. , Lee D.-J. , Lee Y. , Park B.-G. , Pogge R. W. , Ryu Y.-H. , Shin I.-G. , Shvartzvald Y. , Yee J. C. , Zang W. , Zhu W. ,   (KMTNet Collaboration)
Published: April 2018

Abstract
We present Korea Microlensing Telescope Network (KMTNet) light curves for microlensing-event candidates in the Kepler K2 C9 field having peaks within three effective timescales of the Kepler observations. These include 181 “clear microlensing” and 84 “possible microlensing” events found by the KMTNet event finder, plus 56 other events found by OGLE and/or MOA that were not found by KMTNet. All data for the first two classes are immediately available for public use without restriction.
Search for OH 18 cm Radio Emission from 1I/2017 U1 with the Green Bank Telescope
Authors: Park Ryan S. , Pisano D. J. , Lazio T. Joseph W. , Chodas Paul W. , Naidu Shantanu P. 
Published: April 2018

Abstract
This paper reports the first OH 18 cm line observation of the first detected interstellar object 1I/2017 U1 (‘Oumuamua) using the Green Bank Telescope. We have observed the OH lines at 1665.402, 1667.359, and 1720.53 MHz frequencies with a spectral resolution of 357 Hz (approximately 0.06 km s−1). At the time of the observation, ‘Oumuamua was at topocentric distance and velocity of 1.07 au and 63.4 km s−1, respectively, or at heliocentric distance and velocity of 1.8 au and 39 km s−1, respectively. Based on a detailed data reduction and an analogy-based inversion, our final results confirm the asteroidal origin of ‘Oumuamua with an upper bound OH production of Q[OH] < 0.17 × 1028 s−1.
The Dynamics of Truncated Black Hole Accretion Disks. II. Magnetohydrodynamic Case
Authors: Hogg J. Drew , Reynolds Christopher S. 
Published: April 2018

Abstract
We study a truncated accretion disk using a well-resolved, semi-global magnetohydrodynamic simulation that is evolved for many dynamical times (6096 inner disk orbits). The spectral properties of hard-state black hole binary systems and low-luminosity active galactic nuclei are regularly attributed to truncated accretion disks, but a detailed understanding of the flow dynamics is lacking. In these systems the truncation is expected to arise through thermal instability driven by sharp changes in the radiative efficiency. We emulate this behavior using a simple bistable cooling function with efficient and inefficient branches. The accretion flow takes on an arrangement where a “transition zone” exists in between hot gas in the innermost regions and a cold, Shakura & Sunyaev thin disk at larger radii. The thin disk is embedded in an atmosphere of hot gas that is fed by a gentle outflow originating from the transition zone. Despite the presence of hot gas in the inner disk, accretion is efficient. Our analysis focuses on the details of the angular momentum transport, energetics, and magnetic field properties. We find that the magnetic dynamo is suppressed in the hot, truncated inner region of the disk which lowers the effective α-parameter by 65%.
ALMA Observations of the IRDC Clump G34.43+00.24 MM3: Complex Organic and Deuterated Molecules
Authors: Sakai Takeshi , Yanagida Takahiro , Furuya Kenji , Aikawa Yuri , Sanhueza Patricio , Sakai Nami , Hirota Tomoya , Jackson James M. , Yamamoto Satoshi 
Published: April 2018

Abstract
We have observed complex organic molecules (COMs) and deuterated species toward a hot core/corino (HC) associated with the infrared dark cloud clump G34.43+00.24 MM3 with the Atacama Large Millimeter/submillimeter Array. We have detected six normal-COMs (CH3OH, CH3CHO, CH3CH2CN, CH3OCH3, HCOOCH3, and NH2CHO), one deuterated-COM (CH2DCN), and two deuterated fundamental molecules (D2CO and DNC) toward G34.43+00.24 MM3 HC. None of these lines, except for CH3OH, are detected toward the shocked regions in our data, which suggests that COMs do not originate in shocks. The abundance of the COMs relative to CH3OH in G34.43+00.24 MM3 HC is found to be similar to those in high-mass hot cores, rather than those in hot corinos in low-mass star-forming regions. This result suggests that the physical conditions of the warm-up phase of G34.43+00.24 MM3 HC are similar to those of high-mass sources. On the other hand, the D2CO abundance relative to CH3OH in G34.43+00.24 MM3 HC is higher than that of other hot cores, and seems to be comparable to that of hot corinos. The relatively high D2CO/CH3OH ratio of G34.43+00.24 MM3 HC implies a long cold starless phase of G34.43+00.24 MM3 HC.
Global Evolution of an Accretion Disk with a Net Vertical Field: Coronal Accretion, Flux Transport, and Disk Winds
Authors: Zhu Zhaohuan , Stone James M. 
Published: April 2018

Abstract
We report results from global ideal MHD simulations that study thin accretion disks (with thermal scale height H/R = 0.1 and 0.05) threaded by net vertical magnetic fields. Our computations span three orders of magnitude in radius, extend all the way to the pole, and are evolved for more than 1000 innermost orbits. We find that (1) inward accretion occurs mostly in the upper magnetically dominated regions of the disk at z ∼ R, similar to predictions from some previous analytical work and the “coronal accretion” flows found in GRMHD simulations. (2) A quasi-static global field geometry is established in which flux transport by inflows at the surface is balanced by turbulent diffusion. The resulting field is strongly pinched inwards at the surface. A steady-state advection–diffusion model, with a turbulent magnetic Prandtl number of order unity, reproduces this geometry well. (3) Weak unsteady disk winds are launched beyond the disk corona with the Alfvén radius R

A
/R
0 ∼ 3. Although the surface inflow is filamentary and the wind is episodic, we show that the time-averaged properties are well-described by steady-wind theory. Even with strong fields, β
0 = 103 at the midplane initially, only 5% of the angular momentum transport is driven by the wind, and the wind mass flux from the inner decade of the radius is only ∼0.4% of the mass accretion rate. (4) Within the disk, most of the accretion is driven by the Rϕ stress from the MRI and global magnetic fields. Our simulations have many applications to astrophysical accretion systems.
A Strong Limit on the Very-high-energy Emission from GRB 150323A
Authors: Abeysekara A. U. , Archer A. , Benbow W. , Bird R. , Brose R. , Buchovecky M. , Bugaev V. , Connolly M. P. , Cui W. , Errando M. , Falcone A. , Feng Q. , Finley J. P. , Flinders A. , Fortson L. , Furniss A. , Gillanders G. H. , Hütten M. , Hanna D. , Hervet O. , Holder J. , Hughes G. , Humensky T. B. , Johnson C. A. , Kaaret P. , Kar P. , Kelley-Hoskins N. , Kertzman M. , Kieda D. , Krause M. , Krennrich F. , Lang M. J. , Lin T. T. Y. , Maier G. , McArthur S. , Moriarty P. , Mukherjee R. , O’Brien S. , Ong R. A. , Park N. , Perkins J. S. , Petrashyk A. , Pohl M. , Popkow A. , Pueschel E. , Quinn J. , Ragan K. , Reynolds P. T. , Richards G. T. , Roache E. , Rulten C. , Sadeh I. , Santander M. , Sembroski G. H. , Shahinyan K. , Tyler J. , Wakely S. P. , Weiner O. M. , Weinstein A. , Wells R. M. , Wilcox P. , Wilhelm A. , Williams D. A. , Zitzer B. ,   (VERITAS Collaboration), Vurm Indrek , Beloborodov Andrei 
Published: April 2018

Abstract
On 2015 March 23, the Very Energetic Radiation Imaging Telescope Array System (VERITAS) responded to a Swift-Burst Alert Telescope (BAT) detection of a gamma-ray burst, with observations beginning 270 s after the onset of BAT emission, and only 135 s after the main BAT emission peak. No statistically significant signal is detected above 140 GeV. The VERITAS upper limit on the fluence in a 40-minute integration corresponds to about 1% of the prompt fluence. Our limit is particularly significant because the very-high-energy (VHE) observation started only ∼2 minutes after the prompt emission peaked, and Fermi-Large Area Telescope observations of numerous other bursts have revealed that the high-energy emission is typically delayed relative to the prompt radiation and lasts significantly longer. Also, the proximity of GRB 150323A (z = 0.593) limits the attenuation by the extragalactic background light to ∼50% at 100–200 GeV. We conclude that GRB 150323A had an intrinsically very weak high-energy afterglow, or that the GeV spectrum had a turnover below ∼100 GeV. If the GRB exploded into the stellar wind of a massive progenitor, the VHE non-detection constrains the wind density parameter to be A ≳ 3 × 1011 g cm−1, consistent with a standard Wolf–Rayet progenitor. Alternatively, the VHE emission from the blast wave would be weak in a very tenuous medium such as the interstellar medium, which therefore cannot be ruled out as the environment of GRB 150323A.
Discovery of an Extremely Luminous Dust-obscured Galaxy Observed with SDSS, WISE, JCMT, and SMA
Authors: Toba Yoshiki , Ueda Junko , Lim Chen-Fatt , Wang Wei-Hao , Nagao Tohru , Chang Yu-Yen , Saito Toshiki , Kawabe Ryohei 
Published: April 2018

Abstract
We present the discovery of an extremely luminous dust-obscured galaxy (DOG) at z
spec = 3.703, WISE J101326.25+611220.1. This DOG is selected as a candidate of extremely luminous infrared (IR) galaxies based on the photometry from the Sloan Digital Sky Survey and Wide-field Infrared Survey Explorer. In order to derive its accurate IR luminosity, we perform follow-up observations at 450 and 850 μm using the Submillimetre Common User Bolometer Array 2 on the James Clerk Maxwell Telescope, and at 870 and 1300 μm using the Submillimeter Array, which enable us to pin down its IR Spectral Energy Distribution (SED). We perform SED fitting using 14 photometric data (0.4–1300 μm) and estimate its IR luminosity, L
IR (8–1000 μm), to be

×1014
L
☉, making it one of the most luminous IR galaxies in the universe. The energy contribution from an active galactic nucleus (AGN) to the IR luminosity is

%, which indicates that it is an AGN-dominated DOG. On the other hand, its stellar mass (M
*) and star formation rate (SFR) are

=

and

) =

, respectively, which means that this DOG can be considered a starburst galaxy in the M
*–SFR plane. This extremely luminous DOG shows significant AGN and star-forming activity that provides us with an important laboratory to probe the maximum phase of the coevolution of galaxies and supermassive black holes.
A Catalog of Post-starburst Quasars from Sloan Digital Sky Survey Data Release 7
Authors: Wei 魏 Peng 鹏 , Gu 顾 Yang 洋 , Brotherton Michael S. , Shi Yong , Chen Yanmei 
Published: April 2018

Abstract
We present a catalog of nearby (z ≤ 0.5) quasars with significant features of post-starburst stellar populations in their optical spectra: so-called post-starburst quasars, or PSQs. After carefully decomposing spectra from the Sloan Digital Sky Survey (SDSS) Data Release 7 (DR7) Quasar Catalog into quasar and host-galaxy components, we derive a sample of 208 PSQs. Their host-galaxy components have strong Hδ absorption (EW ≥ 6 Å) indicating a significant contribution of an intermediate-aged stellar population formed in a burst of star formation within the past 1 Gyr, which makes them potentially useful for studying the co-evolution of supermassive black holes and their host galaxies.
Properties of Merger Shocks in Merging Galaxy Clusters
Authors: Ha Ji-Hoon , Ryu Dongsu , Kang Hyesung 
Published: April 2018

Abstract
X-ray shocks and radio relics detected in the cluster outskirts are commonly interpreted as shocks induced by mergers of subclumps. We study the properties of merger shocks in merging galaxy clusters, using a set of cosmological simulations for the large-scale structure formation of the universe. As a representative case, we focus on the simulated clusters that undergo almost head-on collisions with mass ratio ∼2. Due to the turbulent nature of the intracluster medium, shock surfaces are not smooth, but composed of shocks with different Mach numbers. As the merger shocks expand outward from the core to the outskirts, the average Mach number,

, increases in time. We suggest that the shocks propagating along the merger axis could be manifested as X-ray shocks and/or radio relics. The kinetic energy through the shocks, F

ϕ
, peaks at ∼1 Gyr after their initial launching, or at ∼1–2 Mpc from the core. Because of the Mach number dependent model adopted here for the cosmic-ray (CR) acceleration efficiency, their CR-energy-weighted Mach number is higher with

, compared to the kinetic-energy-weighted Mach number,

. Most energetic shocks are to be found ahead of the lighter dark matter (DM) clump, while the heavier DM clump is located on the opposite side of clusters. Although our study is limited to the merger case considered, the results such as the means and variations of shock properties and their time evolution could be compared with the observed characteristics of merger shocks, constraining interpretations of relevant observations.
The Formation of a Sunspot Penumbra Sector in Active Region NOAA 12574
Authors: Li Qiaoling , Yan Xiaoli , Wang Jincheng , Kong DeFang , Xue Zhike , Yang Liheng , Cao Wenda 
Published: April 2018

Abstract
We present a particular case of the formation of a penumbra sector around a developing sunspot in the active region NOAA 12574 on 2016 August 11 by using the high-resolution data observed by the New Solar Telescope at the Big Bear Solar Observatory and the data acquired by the Helioseismic and Magnetic Imager and the Atmospheric Imaging Assembly on board the Solar Dynamics Observatory satellite. Before the new penumbra sector formed, the developing sunspot already had two umbrae with some penumbral filaments. The penumbra sector gradually formed at the junction of two umbrae. We found that the formation of the penumbra sector can be divided into two stages. First, during the initial stage of penumbral formation, the region where the penumbra sector formed always appeared blueshifted in a Dopplergram. The area, mean transverse magnetic field strength, and total magnetic flux of the umbra and penumbra sector all increased with time. The initial penumbral formation was associated with magnetic emergence. Second, when the penumbra sector appeared, the magnetic flux and area of the penumbra sector increased after the umbra’s magnetic flux and area decreased. These results indicate that the umbra provided magnetic flux for penumbral development after the penumbra sector appeared. We also found that the newly formed penumbra sector was associated with sunspot rotation. Based on these findings, we suggest that the penumbra sector was the result of the emerging flux that was trapped in the photosphere at the initial stage of penumbral formation, and when the rudimentary penumbra formed, the penumbra sector developed at the cost of the umbra.
UKIRT-2017-BLG-001Lb: A Giant Planet Detected through the Dust
Authors: Shvartzvald Y. , Novati S. Calchi , Gaudi B. S. , Bryden G. , Nataf D. M. , Penny M. T. , Beichman C. , Henderson C. B. , Jacklin S. , Schlafly E. F. , Huston M. J. 
Published: April 2018

Abstract
We report the discovery of a giant planet in event UKIRT-2017-BLG-001, detected by the United Kingdom Infrared Telescope (UKIRT) microlensing survey. The mass ratio between the planet and its host is

, about 1.5 times the Jupiter/Sun mass ratio. The event lies 0.°35 from the Galactic center and suffers from high extinction of A

K
= 1.68. Therefore, it could be detected only by a near-infrared (NIR) survey. The field also suffers from large spatial differential extinction, which makes it difficult to estimate the source properties required to derive the angular Einstein radius. Nevertheless, we find evidence suggesting that the source is located in the far disk. If correct, this would be the first source star of a microlensing event to be identified as belonging to the far disk. We estimate the lens mass and distance using a Bayesian analysis to find that the planet’s mass is

, and it orbits a

star at an instantaneous projected separation of

au. The system is at a distance of

kpc, and so likely resides in the Galactic bulge. In addition, we find a non-standard extinction curve in this field, in agreement with previous results toward high-extinction fields near the Galactic center.
Misaligned Accretion and Jet Production
Authors: King Andrew , Nixon Chris 
Published: April 2018

Abstract
Disk accretion onto a black hole is often misaligned from its spin axis. If the disk maintains a significant magnetic field normal to its local plane, we show that dipole radiation from Lense–Thirring precessing disk annuli can extract a significant fraction of the accretion energy, sharply peaked toward small disk radii R (as R
−17/2 for fields with constant equipartition ratio). This low-frequency emission is immediately absorbed by surrounding matter or refracted toward the regions of lowest density. The resultant mechanical pressure, dipole angular pattern, and much lower matter density toward the rotational poles create a strong tendency to drive jets along the black hole spin axis, similar to the spin-axis jets of radio pulsars, also strong dipole emitters. The coherent primary emission may explain the high brightness temperatures seen in jets. The intrinsic disk emission is modulated at Lense–Thirring frequencies near the inner edge, providing a physical mechanism for low-frequency quasi-periodic oscillations (QPOs). Dipole emission requires nonzero hole spin, but uses only disk accretion energy. No spin energy is extracted, unlike the Blandford–Znajek process. Magnetohydrodynamic/general-relativistic magnetohydrodynamic (MHD/GRMHD) formulations do not directly give radiation fields, but can be checked post-process for dipole emission and therefore self-consistency, given sufficient resolution. Jets driven by dipole radiation should be more common in active galactic nuclei (AGN) than in X-ray binaries, and in low accretion-rate states than high, agreeing with observation. In non-black hole accretion, misaligned disk annuli precess because of the accretor’s mass quadrupole moment, similarly producing jets and QPOs.
Ce que peut apporter la résilience à la prévention des désastres : exemples en Lavours et en Chautagne (Ain, Savoie)
Authors: Pigeon Patrick , Rebotier Julien , Guézo Bernard 
Published: April 2018

L’article justifie l’intérêt et les limites du recours à la notion de résilience, tant pour la recherche que pour la gestion, dans le domaine de la prévention des risques de désastres. Pour ce faire, il mobilise deux sites près du Rhône où l’aléa inondation est comparable (différencié, mais présentant des points communs), l’un à Culoz, près des marais de Lavours, et l’autre en Chautagne, sur la commune de Chanaz, mais où le risque d’inondation est géré de manière opposée. La compréhension du contraste de gestion et de peuplement observé révèle la recomposition de trois approches types de la prévention qui sont : aléa centré, approche territorialisée des risques, et résilience. L’intrication de ces approches successives permet de comprendre pourquoi il peut y avoir autant de définitions différentes de la résilience, leur caractère possiblement contradictoire, et les nombreuses contestations de la notion. Mais elle permet aussi de défendre pourquoi une approche intégrée de la résilience est utile à la compréhension des risques de désastres, tout autant qu’à la gestion. Ainsi envisagée, la résilience permet d’expliciter les apports, en même temps que les limites, des politiques de prévention des risques de désastres.