bluuebunny/crossref_metadata_2025_split huggingface dataset:
Timing of surgery in traumatic brachial plexus injury: a systematic review
Authors: Martin Enrico , Senders Joeky T. , DiRisio Aislyn C. , Smith Timothy R. , Broekman Marike L. D. 
Published: June 2018

OBJECTIVEIdeal timeframes for operating on traumatic stretch and blunt brachial plexus injuries remain a topic of debate. Whereas on the one hand spontaneous recovery might occur, on the other hand, long delays are believed to result in poorer functional outcomes. The goal of this review is to assess the optimal timeframe for surgical intervention for traumatic brachial plexus injuries.METHODSA systematic search was performed in January 2017 in PubMed and Embase databases according to the PRISMA guidelines. Search terms related to “brachial plexus injury” and “timing” were used. Obstetric plexus palsies were excluded. Qualitative synthesis was performed on all studies. Timing of operation and motor outcome were collected from individual patient data. Patients were categorized into 5 delay groups (0–3, 3–6, 6–9, 9–12, and > 12 months). Median delays were calculated for Medical Research Council (MRC) muscle grade ≥ 3 and ≥ 4 recoveries.RESULTSForty-three studies were included after full-text screening. Most articles showed significantly better motor outcome with delays to surgery less than 6 months, with some studies specifying even shorter delays. Pain and quality of life scores were also significantly better with shorter delays. Nerve reconstructions performed after long time intervals, even more than 12 months, can still be useful. All papers reporting individual-level patient data described a combined total of 569 patients; 65.5% of all patients underwent operations within 6 months and 27.4% within 3 months. The highest percentage of ≥ MRC grade 3 (89.7%) was observed in the group operated on within 3 months. These percentages decreased with longer delays, with only 35.7% ≥ MRC grade 3 with delays > 12 months. A median delay of 4 months (IQR 3–6 months) was observed for a recovery of ≥ MRC grade 3, compared with a median delay of 7 months (IQR 5–11 months) for ≤ MRC grade 3 recovery.CONCLUSIONSThe results of this systematic review show that in stretch and blunt injury of the brachial plexus, the optimal time to surgery is shorter than 6 months. In general, a 3-month delay appears to be appropriate because while recovery is better in those operated on earlier, this must be considered given the potential for spontaneous recovery.
Antidepressant use in patients with meningioma: is there an association with tumor recurrence?
Authors: Kohli Karan M. , Loewenstern Joshua , Kessler Remi A. , Pain Margaret , Palmese Christina A. , Bederson Joshua , Shrivastava Raj K. 
Published: June 2018

OBJECTIVEWith increasing general use of antidepressants (ADs), multiple studies have noted a small protective effect of ADs for patients with glioma, but their impact on meningioma has not been established. This study aims to evaluate the role of ADs in the context of additional clinical factors in relation to long-term risk of meningioma recurrence.METHODSOne hundred five patients with an intracranial meningioma presenting from 2011–2014 with at least 3 years of follow-up (median 4.2 years) after resection were reviewed. AD use along with demographics, tumor characteristics, and outcomes were recorded. Multivariate logistic regression was used to analyze the association of AD use with tumor recurrence, including other clinical measures significantly associated with recurrence as covariates.RESULTSTwenty-nine patients (27.4%) were taking ADs (27 selective serotonin reuptake inhibitors, 2 norepinephrine-dopamine reuptake inhibitors) prior to tumor recurrence. Their tumors largely affected the frontal (31.0%) or parietal lobe (17.2%) and were located in convexity, parasagittal, or falcine (CPF) areas more frequently than skull base areas relative to the tumors of non-AD users (p = 0.035). AD use was found to be an independent predictor of recurrence, in addition to subtotal resection and WHO grade II/III classification (p values < 0.05). The median time from AD prescription to tumor recurrence was 36.6 months (interquartile range [IQR] = 20.9–62.9 months) and median length of AD use was 41.4 months (IQR = 24.7–62.8 months).CONCLUSIONSAD use was an independent predictor of meningioma recurrence. This association may be due to mood or affective changes caused by tumor location in CPF regions that may be a sign of early recurrence. The finding calls attention to AD use in the management of patients with meningioma, and warrants further exploration of an underlying relationship.
The role of indocyanine green videoangiography with FLOW 800 analysis for the surgical management of central nervous system tumors: an update
Authors: Acerbi Francesco , Vetrano Ignazio G. , Sattin Tommaso , de Laurentis Camilla , Bosio Lorenzo , Rossini Zefferino , Broggi Morgan , Schiariti Marco , Ferroli Paolo 
Published: June 2018

OBJECTIVEIndocyanine green videoangiography (ICG-VA) is an intraoperative technique used to highlight vessels in neurovascular surgery. Its application in the study of the vascular pathophysiology in CNS tumors and its role in their surgical management are still rather limited. A recent innovation of ICG-VA (i.e., the FLOW 800 algorithm integrated in the surgical microscope) allows a semiquantitative evaluation of cerebral blood flow. The aim of this study was to evaluate for the first time the systematic application of ICG-VA and FLOW 800 analysis during surgical removal of CNS tumors.METHODSBetween May 2011 and December 2017, all cases in which ICG-VA and FLOW 800 analysis were used at least one time before, during, or after the tumor resection, and in which surgical videos were available, were retrospectively reviewed. Results of the histological analysis were analyzed together with the intraoperative ICG-VA with FLOW 800 in order to investigate the tumor-related videoangiographic features.RESULTSSeventy-one patients who underwent surgery for cerebral and spinal tumors were intraoperatively analyzed using ICG-VA with FLOW 800, either before or after tumor resection, for a total of 93 videoangiographic studies. The histological diagnosis was meningioma in 25 cases, glioma in 14, metastasis in 7, pineal region tumor in 5, hemangioblastoma in 4, chordoma in 3, and other histological types in 13 cases. The authors identified 4 possible applications of ICG-VA and FLOW 800 in CNS tumor surgery: extradural surveys allowed exploration of sinus patency and the course of veins before dural opening; preresection surveys helped in identifying pathological vascularization (arteriovenous fistulas and neo-angiogenesis) and regional venous outflow, and in performing temporary venous clipping tests, when necessary; postresection surveys were conducted to evaluate arterial and venous patency and parenchymal perfusion after tumor removal; and a premyelotomy survey was conducted in intramedullary tumors to highlight the posterior median sulcus.CONCLUSIONSThe authors found ICG-VA with FLOW 800 to be a useful method to monitor blood flow in the exposed vessels and parenchyma during microsurgical removal of CNS tumors in selected cases. In particular, a preresection survey provides useful information about pathophysiological changes of brain vasculature related to the tumor and aids in the individuation of helpful landmarks for the surgical approach, and the postresection survey helps to prevent potential complications associated with the resection (such as local hypoperfusion or venous infarction).
Deterministic Meeting of Sniffing Agents in the Plane
Authors: Elouasbi Samir , Pelc Andrzej 
Published: June 2018

Two mobile agents, starting at arbitrary, possibly different times from arbitrary locations in the plane, have to meet. Agents are modeled as discs of diameter 1, and meeting occurs when these discs touch. Agents have different labels which are positive integers. Each agent knows its own label, but not the label of the other agent. Agents are equipped with compasses and have synchronized clocks. They make a series of moves. Each move specifies the direction and the duration of moving. This includes a null move which consists in staying inert for some time, or forever. In a non-null move agents travel at the same constant speed, normalized to 1. We assume that agents have sensors enabling them to estimate the distance from the other agent (defined as the distance between centers of discs), but not the direction towards it. We consider two models of estimation. In both models an agent reads its sensor at the moment of its appearance in the plane and then at the end of each move. This reading (together with the previous ones) determines the decision concerning the next move. In both models the reading of the sensor tells the agent if the other agent is already present. Moreover, in the monotone model, each agent can find out, for any two readings in moments t1 and t2, whether the distance from the other agent at time t1 was smaller, equal or larger than at time t2. In the weaker binary model, each agent can find out, at any reading, whether it is at distance less than ρ or at distance at least ρ from the other agent, for some real ρ > 1 unknown to them. Such distance estimation mechanism can be implemented, e.g., using chemical sensors. Each agent emits some chemical substance (scent), and the sensor of the other agent detects it, i.e., sniffs. The intensity of the scent decreases with the distance. In the monotone model it is assumed that the sensor is ideally accurate and can measure any change of intensity. In the binary model it is only assumed that the sensor can detect the scent below some distance (without being able to measure intensity) above which the scent is too weak to be detected. We show the impact of the two ways of sensing on the cost of meeting, defined as the total distance travelled by both agents until the meeting. For the monotone model we show an algorithm achieving meeting at cost O( D), where D is the initial distance between the agents. This complexity is optimal. For the binary model we show that, if agents start at distance smaller than ρ (i.e., when they sense each other initially) then meeting can be guaranteed at cost O( ρ log λ), where λ is the larger label, and that this cost cannot be improved in general. Finally we observe that, if agents start at distance αρ, for some constant α > 1 in the binary model, then sniffing does not help, i.e., the worst-case optimal meeting cost is of the same order of magnitude as without any sniffing ability.
Location verification algorithm of wearable sensors for wireless body area networks
Authors: Wang Hua , Wen Yingyou , Zhao Dazhe 
Published: June 2018

BACKGROUND: Knowledge of the location of sensor devices is crucial for many medical applications of wireless body area networks, as wearable sensors are designed to monitor vital signs of a patient while the wearer still has the freedom of movement. However, clinicians or patients can misplace the wearable sensors, thereby causing a mismatch between their physical locations and their correct target positions. An error of more than a few centimeters raises the risk of mistreating patients. OBJECTIVE: The present study aims to develop a scheme to calculate and detect the position of wearable sensors without beacon nodes. METHODS: A new scheme was proposed to verify the location of wearable sensors mounted on the patient’s body by inferring differences in atmospheric air pressure and received signal strength indication measurements from wearable sensors. Extensive two-sample [Formula: see text] tests were performed to validate the proposed scheme. RESULTS: The proposed scheme could easily recognize a 30-cm horizontal body range and a 65-cm vertical body range to correctly perform sensor localization and limb identification. CONCLUSIONS: All experiments indicate that the scheme is suitable for identifying wearable sensor positions in an indoor environment.
Dynamic Portrait of the Retrograde 1:1 Mean Motion Resonance
Authors: Huang Yukun , Li Miao , Li Junfeng , Gong Shengping 
Published: June 2018

Abstract
Asteroids in mean motion resonances with giant planets are common in the solar system, but it was not until recently that several asteroids in retrograde mean motion resonances with Jupiter and Saturn were discovered. A retrograde co-orbital asteroid of Jupiter, 2015 BZ509 is confirmed to be in a long-term stable retrograde 1:1 mean motion resonance with Jupiter, which gives rise to our interests in its unique resonant dynamics. In this paper, we investigate the phase-space structure of the retrograde 1:1 resonance in detail within the framework of the circular restricted three-body problem. We construct a simple integrable approximation for the planar retrograde resonance using canonical contact transformation and numerically employ the averaging procedure in closed form. The phase portrait of the retrograde 1:1 resonance is depicted with the level curves of the averaged Hamiltonian. We thoroughly analyze all possible librations in the co-orbital region and uncover a new apocentric libration for the retrograde 1:1 resonance inside the planet’s orbit. We also observe the significant jumps in orbital elements for outer and inner apocentric librations, which are caused by close encounters with the perturber.
Spitzer Opens New Path to Break Classic Degeneracy for Jupiter-mass Microlensing Planet OGLE-2017-BLG-1140Lb
Authors: Novati S. Calchi , Skowron J. , Jung Y. K. , Beichman C. , Bryden G. , Carey S. , Gaudi B. S. , Henderson C. B. , Shvartzvald Y. , Yee J. C. , Zhu W. ,   (Spitzer Team), Udalski A. , Szymański M. K. , Mróz P. , Poleski R. , Soszyński I. , Kozłowski S. , Pietrukowicz P. , Ulaczyk K. , Pawlak M. , Rybicki K. , Iwanek P. ,   (OGLE Collaboration), Albrow M. D. , Chung S.-J. , Gould A. , Han C. , Hwang K.-H. , Ryu Y.-H. , Shin I.-G. , Zang W. , Cha S.-M. , Kim D.-J. , Kim H.-W. , Kim S.-L. , Lee C.-U. , Lee D.-J. , Lee Y. , Park B.-G. , Pogge R. W. ,   (KMTNet Collaboration)
Published: June 2018

Abstract
We analyze the combined Spitzer and ground-based data for OGLE-2017-BLG-1140 and show that the event was generated by a Jupiter-class

planet orbiting a mid-late M dwarf

that lies

in the foreground of the microlensed Galactic-bar source star. The planet–host projected separation is

, i.e., well beyond the snow line. By measuring the source proper motion

from ongoing long-term OGLE imaging and combining this with the lens-source relative proper motion

derived from the microlensing solution, we show that the lens proper motion

is consistent with the lens lying in the Galactic disk, although a bulge lens is not ruled out. We show that while the Spitzer and ground-based data are comparably well fitted by planetary (i.e., binary-lens (2L1S)) and binary-source (1L2S) models, the combination of Spitzer and ground-based data decisively favors the planetary model. This is a new channel to resolve the 2L1S/1L2S degeneracy, which can be difficult to break in some cases.
OSSOS. IX. Two Objects in Neptune's 9:1 Resonance—Implications for Resonance Sticking in the Scattering Population
Authors: Volk Kathryn , Murray-Clay Ruth A. , Gladman Brett J. , Lawler Samantha M. , Yu Tze Yeung Mathew , Alexandersen Mike , Bannister Michele T. , Chen 陳英 Ying-Tung 同 , Dawson Rebekah I. , Greenstreet Sarah , Gwyn Stephen D. J. , Kavelaars J. J. , Lin 林省 Hsing Wen 文 , Lykawka Patryk Sofia , Petit Jean-Marc 
Published: June 2018

Abstract
We discuss the detection in the Outer Solar System Origins Survey (OSSOS) of two objects in Neptune’s distant 9:1 mean motion resonance at semimajor axis a ≈ 130 au. Both objects are securely resonant on 10 Myr timescales, with one securely in the 9:1 resonance’s leading asymmetric libration island and the other in either the symmetric or trailing asymmetric island. These objects are the largest semimajor axis objects with secure resonant classifications, and their detection in a carefully characterized survey allows for the first robust resonance population estimate beyond 100 au. The detection of these objects implies a 9:1 resonance population of 1.1 × 104 objects with H

r
< 8.66 (D ≳ 100 km) on similar orbits (95% confidence range of ∼(0.4–3) × 104). Integrations over 4 Gyr of an ensemble of clones spanning these objects’ orbit-fit uncertainties reveal that they both have median resonance occupation timescales of ∼1 Gyr. These timescales are consistent with the hypothesis that these objects originate in the scattering population but became transiently stuck to Neptune’s 9:1 resonance within the last ∼1 Gyr of solar system evolution. Based on simulations of a model of the current scattering population, we estimate the expected resonance sticking population in the 9:1 resonance to be 1000–4500 objects with H

r
< 8.66; this is marginally consistent with the OSSOS 9:1 population estimate. We conclude that resonance sticking is a plausible explanation for the observed 9:1 population, but we also discuss the possibility of a primordial 9:1 population, which would have interesting implications for the Kuiper Belt’s dynamical history.
OGLE-2015-BLG-1459L: The Challenges of Exo-moon Microlensing
Authors: Hwang K.-H. , Udalski A. , Bond I. A. , Albrow M. D. , Chung S.-J. , Gould A. , Han C. , Jung Y. K. , Ryu Y.-H. , Shin I.-G. , Yee J. C. , Zhu W. , Cha S.-M. , Kim D.-J. , Kim H.-W. , Kim S.-L. , Lee C.-U. , Lee D.-J. , Lee Y. , Park B.-G. , Pogge R. W. ,   (KMTNet Collaboration), Pawlak M. , Poleski R. , Szymański M. K. , Skowron J. , Soszyński I. , Mróz P. , Kozłowski S. , Pietrukowicz P. , Ulaczyk K. ,   (OGLE Collaboration), Abe F. , Asakura Y. , Barry R. , Bennett D. P. , Bhattacharya A. , Donachie M. , Evans P. , Fukui A. , Hirao Y. , Itow Y. , Kawasaki K. , Koshimoto N. , Li M. C. A. , Ling C. H. , Masuda K. , Matsubara Y. , Miyazaki S. , Muraki Y. , Nagakane M. , Ohnishi K. , Ranc C. , Rattenbury N. J. , Saito To. , Sharan A. , Sullivan D. J. , Sumi T. , Suzuki D. , Tristram P. J. , Yamada T. , Yamada T. , Yonehara A. ,   (MOA Collaboration)
Published: June 2018

Abstract
We show that dense OGLE and KMTNet I-band survey data require four bodies (sources plus lenses) to explain the microlensing light curve of OGLE-2015-BLG-1459. However, these can equally well consist of three lenses and one source (3L1S), two lenses and two sources (2L2S), or one lens and three sources (1L3S). In the 3L1S and 2L2S interpretations, the host is a brown dwarf and the dominant companion is a Neptune-class planet, with the third body (in the 3L1S case) being a Mars-class object that could have been a moon of the planet. In the 1L3S solution, the light curve anomalies are explained by a tight (five stellar radii) low-luminosity binary source that is offset from the principal source of the event by

. These degeneracies are resolved in favor of the 1L3S solution by color effects derived from comparison to MOA data, which are taken in a slightly different (R/I) passband. To enable current and future (WFIRST) surveys to routinely characterize exo-moons and distinguish among such exotic systems requires an observing strategy that includes both a cadence faster than 9 minute−1 and observations in a second band on a similar timescale.
Orbital Characteristics of the Subdwarf-B and F V Star Binary EC 20117-4014 (=V4640 Sgr)
Authors: Otani T. , Oswalt T. D. , Lynas-Gray A. E. , Kilkenny D. , Koen C. , Amaral M. , Jordan R. 
Published: June 2018

Abstract
Among the competing evolution theories for subdwarf-B (sdB) stars is the binary evolution scenario. EC 20117-4014 (=V4640 Sgr) is a spectroscopic binary system consisting of a pulsating sdB star and a late F main-sequence companion; however, the period and the orbit semimajor axes have not been precisely determined. This paper presents orbital characteristics of the EC 20117-4014 binary system using 20 years of photometric data. Periodic observed minus calculated (O–C) variations were detected in the two highest-amplitude pulsations identified in the EC 20117-4014 power spectrum, indicating the binary system’s precise orbital period (P = 792.3 days) and the light-travel-time amplitude (A = 468.9 s). This binary shows no significant orbital eccentricity, and the upper limit of the eccentricity is 0.025 (using 3σ as an upper limit). This upper limit of the eccentricity is the lowest among all wide sdB binaries with known orbital parameters. This analysis indicated that the sdB is likely to have lost its hydrogen envelope through stable Roche lobe overflow, thus supporting hypotheses for the origin of sdB stars. In addition to those results, the underlying pulsation period change obtained from the photometric data was

P

˙

= 5.4 (±0.7) × 10−14 d d−1, which shows that the sdB is just before the end of the core helium-burning phase.
Thermodynamic Properties of the Inverse Evershed Flow at Its Downflow Points
Authors: Choudhary D. P. , Beck C. 
Published: June 2018

Abstract
We used spectropolarimetric observations of a sunspot in the active region NOAA 11809 in the Ca ii line at 854.2 nm taken with the SpectroPolarimeter for Optical and Infrared Regions at the Dunn Solar Telescope to infer thermodynamic parameters along 100 super-penumbral fibrils that harbor the inverse Evershed flow. The fibrils were identified in line-of-sight (LOS) velocity and line–core intensity maps. The chromospheric LOS velocity abruptly decreases from 3 to 15 km s−1 to zero at the inner footpoints of the fibrils that are located from the mid penumbra to about 1.4 spot radii. The spectra often show multiple absorption components, indicating spatially or vertically unresolved structures. Synthetic spectra with a 100% fill factor of a flow channel in the upper atmosphere yield strongly asymmetric profiles but no multiple separate components. The line–core intensity always peaks slightly closer to the umbra than the LOS velocity. Using the CAlcium Inversion using a Spectral ARchive code, we find that the fibrils make an angle of 30°–60° to the local vertical away from the umbra. The temperature near the downflow points is enhanced by 200 K at log

and up to 2000 K at log τ ∼ (−6) compared to the quiet Sun, without any signature in the low photosphere. Our results are consistent with a critical, i.e., sonic, or supersonic siphon flow along super-penumbral flux tubes in which accelerating plasma abruptly attains subcritical velocity through a standing shock in or near the penumbra.
A VLA Study of High-redshift GRBs. II. The Complex Radio Afterglow of GRB 140304A: Shell Collisions and Two Reverse Shocks
Authors: Laskar Tanmoy , Berger Edo , Margutti Raffaella , Zauderer B. Ashley , Williams Peter K. G. , Fong Wen-fai , Sari Re’em , Alexander Kate D. , Kamble Atish 
Published: June 2018

Abstract
We present detailed multifrequency, multiepoch radio observations of GRB 140304A at z = 5.283 from 1 to 86 GHz and from 0.45 to 89 days. The radio and millimeter data exhibit unusual multiple spectral components, which cannot be simply explained by standard forward and reverse shock scenarios. Through detailed multiwavelength analysis spanning radio to X-rays, we constrain the forward shock parameters to E
k,iso ≈ 4.9 × 1054 erg,

A

*

≈ 2.6 × 10−2,

ϵ

e

≈ 2.5 × 10−2,

ϵ

B

≈ 5.9 × 10−2, p ≈ 2.6, and

θ

jet

≈ 1.°1, yielding a beaming-corrected γ-ray and kinetic energy,

E

γ

≈ 2.3 × 1049 erg and

E

K

≈ 9.5 × 1050 erg, respectively. We model the excess radio emission as due to a combination of a late-time reverse shock (RS) launched by a shell collision, which also produces a rebrightening in the X-rays at ≈0.26 days, and either a standard RS or diffractive interstellar scintillation (ISS). Under the standard RS interpretation, we invoke consistency arguments between the forward and reverse shocks to derive a deceleration time, t
dec ≈ 100 s, the ejecta Lorentz factor, Γ(t
dec) ≈ 300, and a low RS magnetization, R
B ≈ 0.6. Our observations highlight both the power of radio observations in capturing RS emission and thus constraining the properties of GRB ejecta and central engines and the challenge presented by ISS in conclusively identifying RS emission in GRB radio afterglows.