bluuebunny/crossref_metadata_2025_split huggingface dataset:
Adenosine-induced cardiac arrest as an alternative to temporary clipping during intracranial aneurysm surgery
Authors: Intarakhao Patcharin , Thiarawat Peeraphong , Rezai Jahromi Behnam , Kozyrev Danil A. , Teo Mario K. , Choque-Velasquez Joham , Luostarinen Teemu , Hernesniemi Juha 
Published: October 2017

OBJECTIVEThe purpose of this study was to analyze the impact of adenosine-induced cardiac arrest (AiCA) on temporary clipping (TC) and the postoperative cerebral infarction rate among patients undergoing intracranial aneurysm surgery.METHODSIn this retrospective matched-cohort study, 65 patients who received adenosine for decompression of aneurysms during microsurgical clipping were identified (Group A) and randomly matched with 65 selected patients who underwent clipping but did not receive adenosine during surgery (Group B). The matching criteria included age, Fisher grade, aneurysm size, rupture status, and location of aneurysms. The primary outcomes were TC time and the postoperative infarction rate. The secondary outcome was the incidence of intraoperative aneurysm rupture (IAR).RESULTSIn Group A, 40 patients underwent clipping with AiCA alone and 25 patients (38%) received AiCA combined with TC, and in Group B, 60 patients (92%) underwent aneurysm clipping under the protection of TC (OR 0.052; 95% CI 0.018–0.147; p < 0.001). Group A required less TC time (2.04 minutes vs 4.46 minutes; p < 0.001). The incidence of postoperative lacunar infarction was equal in both groups (6.2%). There was an insignificant between-group difference in the incidence of IAR (1.5% in Group A vs 6.1% in Group B; OR 0.238; 95% CI 0.026–2.192; p = 0.171).CONCLUSIONSAiCA is a useful technique for microneurosurgical treatment of cerebral aneurysms. AiCA can minimize the use of TC and does not increase the risk of IAR and postoperative infarction.
Direct versus indirect revascularization in the treatment of moyamoya disease
Authors: Park Seong-eun , Kim Ju-seong , Park Eun Kyung , Shim Kyu-Won , Kim Dong-Seok 
Published: October 2017

OBJECTIVEFor patients with moyamoya disease (MMD), surgical intervention is usually required because of progressive occlusion of the internal carotid artery. The indirect bypass method has been widely accepted as the treatment of choice in pediatric patients. However, in adult patients with MMD, the most effective treatment method remains a matter of debate. Here, the authors compared the clinical outcomes from MMD patients treated with either extracranial-intracranial arterial bypass (EIAB; 43 hemispheres) or modified encephaloduroarteriosynangiosis (mEDAS; 75 hemispheres) to investigate whether mEDAS is an effective surgical method for treating adults with symptomatic MMD.METHODSA comparative analysis was performed in patients treated using either mEDAS or EIAB. Collateral grading, collateral vein counting, and symptom analysis were used to assess the outcome of surgery.RESULTSSeventy-seven percent (58/75) of mEDAS cases and 83.7% (36/43) of EIAB cases in the analysis experienced improvement in their symptoms after surgery. Furthermore, patients in 98.7% (74/75) of mEDAS cases and those in 95.3% (41/43) of EIAB cases exhibited improved collateral grades. Increases in regions of perfusion were seen after both procedures.CONCLUSIONSModified EDAS and EIAB both result in positive outcomes for symptomatic adults with MMD. However, when considering the benefit of both surgeries, the authors propose mEDAS, a simpler and less strenuous surgery with a lower risk of complications, as a sufficient and safe treatment option for symptomatic adults with MMD.
Surgical site infection after transoral versus posterior approach for atlantoaxial fusion: a matched-cohort study
Authors: Macki Mohamed , Basheer Azam , Lee Ian , Kather Ryan , Rubinfeld Ilan , Abdulhak Muwaffak M. 
Published: October 2017

OBJECTIVEIn the past, spine surgeons have avoided the transoral approach to the atlantoaxial segment because of concerns for unacceptable patient morbidity. The objective of this study was to measure 30-day postoperative complications, especially surgical site infection (SSI), after transoral versus posterior approach to atlantoaxial fusion.METHODSThe source population was provided by the American College of Surgeons National Surgical Quality Improvement Program database, which was queried for all patients who underwent atlantoaxial fusion for degenerative/spondylotic disease and/or trauma between 2005 and 2014. To eliminate bias from unequal sample sizes, patients who underwent the transoral approach were matched with patients who underwent the posterior approach (generally 1:5 ratio) based on age ± 5 years and modified frailty index score (a measure of preoperative comorbidity burden). Because of rare SSI incidence, adjusted odds ratios (ORadj) of SSI were calculated using penalized maximum likelihood estimation.RESULTSA total of 318 patients were included in the study. There were no statistically significant differences between the transoral cohort (n = 56) and the posterior cohort (n = 262) in terms of 30-day postoperative individual complications, including SSI (1.79% vs 1.91%; p = 0.951) and composite complications (10.71% vs 6.87%; p = 0.323). Controlling for sex and smoking, the odds of SSI in the transoral approach were almost equal to the odds in the posterior approach (ORadj 1.17; p = 0.866). While the unplanned reoperation rate of 5.36% after transoral surgery was higher than the 1.53% rate after posterior surgery, the difference approached, but did not reach, statistical significance (p = 0.076).CONCLUSIONSTransoral versus posterior surgery for atlantoaxial fusion did not differ in 30-day unexpected outcomes. Therefore, spinal pathology, rather than concern for postoperative complications, should adjudicate the technical approach to the atlantoaxial segment.
Prevalence of Clostridium Difficile Infection in Patients After Radical Cystectomy and Neoadjuvant Chemotherapy
Authors: Cotter Katherine J. , Fan Yunhua , Sieger Gretchen K. , Weight Christopher J. , Konety Badrinath R. 
Published: October 2017

Background and Objectives: Clostridium Difficile is the most common cause of nosocomial infectious diarrhea. This study evaluates the prevalence and predictors of Clostridium Difficile infections in patients undergoing radical cystectomy with or without neoadjuvant chemotherapy. Methods: Retrospective chart review was performed of all patients undergoing cystectomy and urinary diversion at a single institution from 2011–2017. Infection was documented in all cases with testing for Clostridium Difficile polymerase chain reaction toxin B. Patient and disease related factors were compared for those who received neoadjuvant chemotherapy vs. those who did not in order to identify potential risk factors associated with C. Difficile infections. Chi squared test and logistic regression analysis were used to determine statistical significance. Results: Of 350 patients who underwent cystectomy, 41 (11.7%) developed Clostridium Difficile in the 30 day post-operative period. The prevalence of C. Difficile infection was higher amongst the patients undergoing cystectomy compared to the non-cystectomy admissions at our hospital (11.7 vs. 2.9%). Incidence was not significantly different among those who underwent cystectomy for bladder cancer versus those who underwent the procedure for other reasons. Median time to diagnosis was 6 days (range 3–28 days). The prevalence of C. Diff infections was not significantly different among those who received neoadjuvant chemotherapy vs. those who did not (11% vs. 10.4% p = 0.72). A significant association between C. Difficile infection was not seen with proton pump inhibitor use ( p = 0.48), patient BMI ( p = 0.67), chemotherapeutic regimen ( p = 0.94), individual surgeon ( p = 0.54), type of urinary diversion (0.41), or peri-operative antibiotic redosing ( p = 0.26). Conclusions: Clostridium Difficile infection has a higher prevalence in patients undergoing cystectomy. No significant association between prevalence and exposure to neoadjuvant chemotherapy was seen.
Long-term Study of the Solar Filaments from the Synoptic Maps as Derived from
Spectroheliograms of the Kodaikanal Observatory
Authors: Chatterjee Subhamoy , Hegde Manjunath , Banerjee Dipankar , Ravindra B. 
Published: October 2017

Abstract
The century long (1914–2007)

(656.28 nm) spectroheliograms from the Kodaikanal Solar Observatory (KSO) have been recently digitized. Using these newly calibrated, processed images we study the evolution of dark elongated on-disk structures called filaments, which are potential representatives of magnetic activities on the Sun. To our knowledge, this is the oldest uniform digitized data set with daily images available today in

. We generate Carrington maps for the entire time duration and try to find the correlations with maps of the same Carrington rotation from the Ca ii K KSO data. Filaments are segmented from the Carrington maps using a semi-automated technique and are studied individually to extract their centroids and tilts. We plot the time-latitude distribution of the filament centroids, producing a butterfly diagram which clearly shows the presence of poleward migration. We separate polar filaments for each cycle and try to estimate the delay between the polar filament number cycle and the sunspot number cycle peaks. We correlate this delay with the delay between polar reversal and sunspot number maxima. This provides new insight on the role of polar filaments on polar reversal.
Multiple-wavelength Variability and Quasi-periodic Oscillation of PMN J0948+0022
Authors: Zhang Jin , Zhang Hai-Ming , Zhu Yong-Kai , Yi Ting-Feng , Yao Su , Lu Rui-Jing , Liang En-Wei 
Published: October 2017

Abstract
We present a comprehensive analysis of multiple-wavelength observational data of the first GeV-selected narrow-line Seyfert 1 galaxy PMN J0948+0022. We derive its light curves in the γ-ray and X-ray bands from the data observed with Fermi/LAT and Swift/XRT, and generate the optical and radio light curves by collecting the data from the literature. These light curves show significant flux variations. With the LAT data we show that this source is analogous to typical flat spectrum radio quasars in the L

γ
–Γ
γ
plane, where L

γ
and Γ
γ
are the luminosity and spectral index in the LAT energy band. The γ-ray flux is correlated with the V-band flux with a lag of ∼44 days, and a moderate quasi-periodic oscillation (QPO) with a periodicity of ∼490 days observed in the LAT light curve. A similar QPO signature is also found in the V-band light curve. The γ-ray flux is not correlated with the radio flux in 15 GHz, and no similar QPO signature is found at a confidence level of 95%. Possible mechanisms of the QPO are discussed. We propose that gravitational-wave observations in the future may clarify the current plausible models for the QPO.
The Interstellar Medium in [O iii]-selected Star-forming Galaxies at z ∼ 3.2
Authors: Suzuki Tomoko L. , Kodama Tadayuki , Onodera Masato , Shimakawa Rhythm , Hayashi Masao , Tadaki Ken-ichi , Koyama Yusei , Tanaka Ichi , Sobral David , Smail Ian , Best Philip N. , Khostovan Ali A. , Minowa Yosuke , Yamamoto Moegi 
Published: October 2017

Abstract
We present new results from near-infrared spectroscopy with Keck/MOSFIRE of [O iii]-selected galaxies at

z
∼
3.2

. With our H and K band spectra, we investigate the interstellar medium (ISM) conditions, such as ionization states and gas metallicities. [O iii] emitters at

z
∼
3.2

show a typical gas metallicity of

12
+
log
(
O

/

H
)
=
8.07
±
0.07

at

log
(

M

*

/

M

⊙

)

∼

9.0
–
9.2

and

12
+
log
(
O

/

H
)
=
8.31
±
0.04

at

log
(

M

*

/

M

⊙

)

∼

9.7
–
10.2

when using the empirical calibration method. We compare the [O iii] emitters at

z
∼
3.2

with UV-selected galaxies and Lyα emitters at the same epoch and find that the [O iii]-based selection does not appear to show any systematic bias in the selection of star-forming galaxies. Moreover, comparing with star-forming galaxies at

z
∼
2

from the literature, our samples show similar ionization parameters and gas metallicities as those obtained by the previous studies that used the same calibration method. We find no strong redshift evolution in the ISM conditions between

z
∼
3.2

and

z
∼
2

. Considering that the star formation rates at a fixed stellar mass also do not significantly change between the two epochs, our results support the idea that the stellar mass is the primary quantity to describe the evolutionary stages of individual galaxies at

z
>
2

.
Convection and Overshoot in Models of γ Doradus and δ Scuti Stars
Authors: Lovekin C. C. , Guzik J. A. 
Published: October 2017

Abstract
We investigate the pulsation properties of stellar models that are representative of δ Scuti and γ Doradus variables. We have calculated a grid of stellar models from 1.2 to 2.2 M
⊙, including the effects of both rotation and convective overshoot using MESA, and we investigate the pulsation properties of these models using GYRE. We discuss the observable patterns in the frequency spacing for p modes and the period spacings for g modes. Using the observable patterns in the g mode period spacings, it may be possible to observationally constrain the convective overshoot and rotation of a model. We also calculate the pulsation constant (Q) for all models in our grid and investigate the variation with convective overshoot and rotation. The variation in the Q values of the radial modes can be used to place constraints on the convective overshoot and rotation of stars in this region. As a test case, we apply this method to a sample of 22 High-Amplitude δ Scuti stars (HADS) and provide estimates for the convective overshoot of the sample.
The Role of the CMB in Redshift Related Departures from the Gao–Solomon Relation
Authors: Tunnard R. , Greve T. R. 
Published: October 2017

Abstract
A strong correlation between the far-IR and HCN(1−0) line luminosities, known as the Gao–Solomon relation, has been observed to hold over more than 10 orders of magnitude in the local universe. Departures from this relation at redshifts ≳1.5 have been interpreted as evidence for increased dense gas star formation efficiency in luminous galaxies during the period of peak of star formation in the history of the universe. We examine whether the offsets from the relation can be explained by the hotter Cosmic Microwave Background (CMB) at high redshift, which, due to a loss of contrast against the hotter background, reduces the observable molecular-line flux far more significantly than the far-IR continuum bands. Simple line-of-sight modeling argues for highly significant departures from the Gao–Solomon relation at high redshift for kinetic temperatures ∼15 K, while more complex toy-galaxy models based on NGC 1068 suggest a much weaker effect with the galaxy integrated HCN line flux falling by only 10% at z = 3, within the intrinsic scatter of the relation. We conclude that, while the CMB is unlikely to explain the deviations reported in the literature, it may introduce a second-order effect on the relation by raising the low-luminosity end of the Gao–Solomon relation in cooler galaxies. A similar examination of the CO-IR relation finds tantalizing signs of the CMB having a measurable effect on the integrated CO emission in high-redshift galaxies, but these signs cannot be confirmed with the current data.
Particle Acceleration and Fractional Transport in Turbulent Reconnection
Authors: Isliker Heinz , Pisokas Theophilos , Vlahos Loukas , Anastasiadis Anastasios 
Published: October 2017

Abstract
We consider a large-scale environment of turbulent reconnection that is fragmented into a number of randomly distributed unstable current sheets (UCSs), and we statistically analyze the acceleration of particles within this environment. We address two important cases of acceleration mechanisms when particles interact with the UCS: (a) electric field acceleration and (b) acceleration by reflection at contracting islands. Electrons and ions are accelerated very efficiently, attaining an energy distribution of power-law shape with an index 1–2, depending on the acceleration mechanism. The transport coefficients in energy space are estimated from test-particle simulation data, and we show that the classical Fokker–Planck (FP) equation fails to reproduce the simulation results when the transport coefficients are inserted into it and it is solved numerically. The cause for this failure is that the particles perform Levy flights in energy space, while the distributions of the energy increments exhibit power-law tails. We then use the fractional transport equation (FTE) derived by Isliker et al., whose parameters and the order of the fractional derivatives are inferred from the simulation data, and solving the FTE numerically, we show that the FTE successfully reproduces the kinetic energy distribution of the test particles. We discuss in detail the analysis of the simulation data and the criteria that allow one to judge the appropriateness of either an FTE or a classical FP equation as a transport model.
Correlation between X-Ray and Radio Absorption in Compact Radio Galaxies
Authors: Ostorero Luisa , Morganti Raffaella , Diaferio Antonaldo , Siemiginowska Aneta , Stawarz Łukasz , Moderski Rafal , Labiano Alvaro 
Published: October 2017

Abstract
Compact radio galaxies with a GHz-peaked spectrum (GPS) and/or compact-symmetric-object (CSO) morphology (GPS/CSOs) are increasingly detected in the X-ray domain. Their radio and X-ray emissions are affected by significant absorption. However, the locations of the X-ray and radio absorbers are still debated. We investigated the relationship between the column densities of the total (

) and neutral (

) hydrogen to statistically constrain the picture. We compiled a sample of GPS/CSOs including both literature data and new radio data that we acquired with the Westerbork Synthesis Radio Telescope for sources whose X-ray emission was either established or under investigation. In this sample, we compared the X-ray and radio hydrogen column densities, and found that

and

display a significant positive correlation with

∝

b
, where b = 0.47 and b = 0.35, depending on the subsample. The

–

correlation suggests that the X-ray and radio absorbers are either co-spatial or different components of a continuous structure. The correlation displays a large intrinsic spread that we suggest to originate from fluctuations, around a mean value, of the ratio between the spin temperature and the covering factor of the radio absorber,

.
Galactic Latitude Dependence of Near-infrared Diffuse Galactic Light: Thermal Emission or Scattered Light?
Authors: Sano K. , Matsuura S. 
Published: October 2017

Abstract
Near-infrared (IR) diffuse Galactic light (DGL) consists of scattered light and thermal emission from interstellar dust grains illuminated by the interstellar radiation field (ISRF). At 1.25 and

, a recent observational study shows that intensity ratios of the DGL to interstellar

dust emission steeply decrease toward high Galactic latitudes (b). In this paper, we investigate the origin(s) of the b-dependence on the basis of models of thermal emission and scattered light. Combining a thermal emission model with the regional variation of the polycyclic aromatic hydrocarbon abundance observed with Planck, we show that the contribution of the near-IR thermal emission component to the observed DGL is lower than

. We also examine the b-dependence of the scattered light, assuming a plane–parallel Galaxy with smooth distributions of the ISRF and dust density along the vertical direction, and assuming a scattering phase function according to a recently developed model of interstellar dust. We normalize the scattered light intensity to the

intensity corrected for deviation from the cosecant-b law according to the Planck observation. As the result, the present model that considers the b-dependence of dust and the ISRF properties can account for the observed b-dependence of the near-IR DGL. However, the uncertainty in the correction for the

emission is large, and other normalizing quantities may be appropriate for a more robust analysis of the DGL.
Steamworlds: Atmospheric Structure and Critical Mass of Planets Accreting Icy Pebbles
Authors: Chambers John 
Published: October 2017

Abstract
In the core accretion model, gas-giant planets first form a solid core, which then accretes gas from a protoplanetary disk when the core exceeds a critical mass. Here, we model the atmosphere of a core that grows by accreting ice-rich pebbles. The ice fraction of pebbles evaporates in warm regions of the atmosphere, saturating it with water vapor. Excess water precipitates to lower altitudes. Beneath an outer radiative region, the atmosphere is convective, following a moist adiabat in saturated regions due to water condensation and precipitation. Atmospheric mass, density, and temperature increase with core mass. For nominal model parameters, planets with core masses (ice + rock) between 0.08 and 0.16 Earth masses have surface temperatures between 273 and 647 K and form an ocean. In more massive planets, water exists as a supercritical convecting fluid mixed with gas from the disk. Typically, the core mass reaches a maximum (the critical mass) as a function of the total mass when the core is 2–5 Earth masses. The critical mass depends in a complicated way on pebble size, mass flux, and dust opacity due to the occasional appearance of multiple core-mass maxima. The core mass for an atmosphere of 50% hydrogen and helium may be a more robust indicator of the onset of gas accretion. This mass is typically 1–3 Earth masses for pebbles that are 50% ice by mass, increasing with opacity and pebble flux and decreasing with pebble ice/rock ratio.
Charles Walbrou, « Je préférerais ne pas », le réfractaire de l’« Homme mort »
Authors: Ribeill Georges 
Published: October 2017

L’histoire de la lutte contre la va (veille automatique) puis contre la vacma (veille automatique à contrôle de maintien d’appui) se confond avec l’histoire militante d’un cheminot, conducteur de train syndicaliste à la Cftc puis à la Cfdt , Charles Walbrou. Retracer sa vie militante, c’est parcourir cette lutte depuis ses prémices, au début des années 1960, jusqu’à son abandon par les organisations syndicales au détour de mai 1968 avec la priorité donnée aux revendications « générales ». Mais, pour Walbrou, le combat contre la vacma ne s’arrête pas. Ni sa retraite ni l’abandon de cette revendication par les syndicats ne l’empêcheront de poursuivre sa dénonciation de ce système qui « colle l’homme à la machine ».
Une mise en veille de la santé et de la sécurité ou les paradoxes du dispositif d’« Homme mort » sur les tramways
Authors: Doniol-Shaw Ghislaine , Foot Robin , Franchi Pierre 
Published: October 2017

Le milieu du tramway tend à généraliser un dispositif de veille, une vacma (veille automatique à contrôle de maintien d’appui) qui soumet le travail de conduite à une contrainte temporelle forte sans rapport avec la conduite. Le conducteur ne peut maintenir la veille plus de douze secondes. Avant ce délai, il doit relâcher la veille sinon une alarme sonore se déclenche et un freinage d’urgence peut se déclencher. Or, on constate que la majorité des conducteurs tend à intensifier les actions sur la veille, à adopter une fréquence d’action beaucoup plus élevée que ce que le système permet en théorie. Comprendre les raisons de cette stratégie permet d’éclairer la double contrainte qui met sous tension le travail de conduite : préserver sa santé au détriment de l’attention portée à la conduite ou prendre sur soi pour assurer au mieux la sécurité de conduite.