bluuebunny/crossref_metadata_2025_split huggingface dataset:
Volumetric changes and clinical outcome for petroclival meningiomas after primary treatment with Gamma Knife radiosurgery
Authors: Sadik Zjiwar H. A. , Lie Suan Te , Leenstra Sieger , Hanssens Patrick E. J. 
Published: January 2018

OBJECTIVEPetroclival meningiomas (PCMs) can cause devastating clinical symptoms due to mass effect on cranial nerves (CNs); thus, patients harboring these tumors need treatment. Many neurosurgeons advocate for microsurgery because removal of the tumor can provide relief or result in symptom disappearance. Gamma Knife radiosurgery (GKRS) is often an alternative for surgery because it can cause tumor shrinkage with improvement of symptoms. This study evaluates qualitative volumetric changes of PCM after primary GKRS and its impact on clinical symptoms.METHODSThe authors performed a retrospective study of patients with PCM who underwent primary GKRS between 2003 and 2015 at the Gamma Knife Center of the Elisabeth-Tweesteden Hospital in Tilburg, the Netherlands. This study yields 53 patients. In this study the authors concentrate on qualitative volumetric tumor changes, local tumor control rate, and the effect of the treatment on trigeminal neuralgia (TN).RESULTSLocal tumor control was 98% at 5 years and 93% at 7 years (Kaplan-Meier estimates). More than 90% of the tumors showed regression in volume during the first 5 years. The mean volumetric tumor decrease was 21.2%, 27.1%, and 31% at 1, 3, and 6 years of follow-up, respectively. Improvement in TN was achieved in 61%, 67%, and 70% of the cases at 1, 2, and 3 years of follow-up, respectively. This was associated with a mean volumetric tumor decrease of 25% at the 1-year follow-up to 32% at the 3-year follow-up.CONCLUSIONSGKRS for PCMs yields a high tumor control rate with a low incidence of neurological deficits. Many patients with TN due to PCM experienced improvement in TN after radiosurgery. GKRS achieves significant volumetric tumor decrease in the first years of follow-up and thereafter.
Placement of baclofen pump catheter through a C1–2 puncture: technical note
Authors: Aljuboori Zaid , Archer Jacob , Huff Wei , Moreno Amee , Jea Andrew 
Published: January 2018

Intrathecal baclofen has been suggested as an effective and safe treatment for intractable spasticity and dystonia. Techniques of lumbar and intraventricular catheter placement have been previously described. The purpose of this study was to describe a technique to implant catheters for intrathecal baclofen infusion through C1–2 puncture.Four of 5 consecutively treated patients underwent successful placement of catheters for intrathecal baclofen. There were no instances of infection, CSF leak, or catheter migration seen during a follow-up period of at least 6 months; furthermore, there were no occurrences of vertebral artery or spinal cord injury. All patients had an effective stabilization or reduction of their upper-extremity, lower-extremity, or trunk tone. There were no cases of worsening hypertonia.The authors’ preliminary experience with C1–2 puncture for placement of the intrathecal baclofen catheter seems to indicate that this is a safe and efficacious technique. Lessons learned from the failed attempt at C1–2 puncture will be delineated.
Effect of Different Levels of Urea Super Granule and Prilled Urea on the Crop Quality, Nutrient Uptake and Soil Nutrient Status of Broccoli
Authors: Hussain M J , Karim A J M S , Solaiman A R M , Islam M S , Rahman M 
Published: January 2018

A field experiment was conducted at Bangabandhu Sheikh Mujibur Rahman Agricultural University, Gazipur during the period 2010-2011 to assess the effect of urea super granule (USG) and prilled urea (PU) on the quality attributes (Compactness coefficient, Vitamin C, β-carotene and chlorophyll contents) of broccoli, to assess the comparative performance of USG and PU on nutrient uptake and uptake efficiency of broccoli plant, to assess the effect of different forms and levels of urea N on the post harvest soil nutrient status of broccoli field and to select the better doses of USG and PU for quality broccoli production in Shallow Red-Brown Terrace Soil under Madhupur Tract (AEZ-28). The experiment was laid out in a randomized complete block design with three replications having 17 treatments constituted with different levels of urea super granule (USG) and prilled urea (PU) as- T1: N-control, T2: PU-N80, T3: PU-N100, T4: PU-N120, T5: PU-N140, T6: PU-N160, T7: PU-N180, T8: PU-N200, T9: PU-N220, T10: USG-N80, T11: USG-N100, T12: USG-N120, T13: USG-N140, T14: USG-N160, T15: USG-N180, T16: USG-N200, T17 and USG-N220 kg ha-1. Results revealed that the comparative performance of USG in relation to head quality (compactness coefficient, ascorbic acid, β-carotene and chlorophyll content), nutrient (NPKS) uptake and N uptake efficiency was found better as compared to PU. The compactness coefficient, β-carotene and chlorophyll contents were increased with increasing rate of N as well as USG and PU, but ascorbic acid content was slightly decreased with increasing rate of USG and PU. The maximum compactness coefficient (18.61) was found from the treatment USG-N180 that was followed by USG-N160 (18.24) and the highest β-carotene content (0.401 mg/100gFW) was found from USG-N160 followed by PU-N180 (0.40 mg/100gFW). Similarly the highest chlorophyll-a content (0.818 mg/100gFW) was found from USG-N180 followed by USG-N160 (0.814 mg/100gFW) and the highest chlorophyll-b content (1.141mg/100g FW) was recorded from USG-N180. The higher nutrient uptake and N uptake efficiency (108.531%) was obtained from USG treated plots over that of the PU. But N uptake efficiency was decreased with increasing rates of N fertilizer. But post harvest soil nitrogen status did not show any systematic trend although it was found higher in USG over PU. Similarly no remarkable changes were observed in post harvest soil P, K, S and B status for the crop. However, USG @ 160 kg N ha-1 (USG-N160) followed by USG-N140 and PU @ 180 kg N ha-1 (PU-N180) with other recommended doses of fertilizer could be suggested as USG and PU based fertilizer recommendation for a good quality broccoli production in terms of yield and quality in Silty Clay Loam Soil of Madhupur Tract.The Agriculturists 2017; 15(2) 24-39
Point de vue sur l'évolution récente de la spéléologie : conséquences sur l'exploration et la recherche scientifique
Authors: Maire Richard 
Published: January 2018

Depuis 20 à 30 ans, la spéléologie mondiale a fait des
progrès immenses. En 1975, seuls 3 gouffres situés en France (Berger, Pierre Saint-Martin, Jean-Bernard) dépassaient 1 000 m de profondeur. En 1980, on en comptait 11 et début 1995, une cinquantaine ! Ce "boom" des explorations est lié à un ensemble de facteurs : facilités de déplacement, développement des expéditions à l'étranger, techniques de désobstruction, développement de la plongée, publication des résultats, étude des topographies. Le point de départ correspond à la mise au point en France des techniques alpines (progression sur corde simple) et leur application dans des cavités profondes et difficiles dès la fin des années 60 (Vercors, Chartreuse, Pyrénées) provoquant une révolution dans les mentalités. Sur le plan scientifique, cette évolution accélérée des explorations spéléologiques a beaucoup apporté. Grâce aux topographies des cavités et à l'addition progressive de nouveaux passages, on voit les réseaux souterrains s'agrandir. Ces données irremplaçables constituent un moyen objectif pour comprendre l'organisation des systèmes karstiques, même si certains s'emploient à dire que les réseaux souterrains explorés ne représentent qu'une faible partie de la réalité. De plus en plus, on remarque que les réseaux alpins sont souvent assez vieux, certains étant sans doute antérieurs aux glaciations quaternaires. Dans les karsts tropicaux, les recherches ont également fait des progrès importants, notamment dans trois pays pilotes : le Mexique (avec sept -1 000), la Papouasie Nouvelle-Guinée (avec ses puits et torrents souterrains sous la jungle équatoriale, et son 1er -1 000), et surtout la Chine avec ses karsts et ses grottes-tunnels légendaires. Enfin, c'est la plongée souterraine qui aujourd'hui fait des progrès spectaculaires. En plus des siphons très longs explorés au cours des années 80, la plongée aux mélanges a permis d'atteindre des profondeurs étonnantes (Sheck EXLEY) : -262 m à Bushmangat (Afrique du Sud) et -267 m dans la source vauclusienne du Rio Mante (Mexique) sondée jusqu'à -329 m ! Il faut rendre hommage au courage et à la grande technicité des plongeurs qui ont fait faire un bond remarquable dans la recherche spéléologique. En spéléologie alpine, la prochaine révolution technique qui s'amorce déjà viendra entre autres d'un allégement conséquent du matériel.
Optical Photometric Monitoring for 3C 66A during 1996–2009 and Its Periodicity Analysis
Authors: Fan J. H. , Tao J. , Liu Y. , Yuan Y. H. , Sawangwit Utane , Yang J. H. , Huang Y. , Zhang Y. T. , Zhang J. Y. , Zhang L. X. , Zhu J. T. 
Published: January 2018

Abstract
3C 66A is one of the most interesting blazars and one of our monitoring objects carried out with the 1.56 m telescope at Sheshan station, Shanghai Astronomical Observatory (ShAO). It has been monitored since 1996 December 11. In the present work, we show its optical light curves during the period of 1996 December 11–2009 December 28. From our observations, we found that the largest variations in the V, R, and I bands are

,

mag, and ΔI = 1.659 ± 0.047 mag, respectively. Intra-day variabilities are found in the three bands: in the V band, an A = 17.7% brightness increase over

minutes on JD 2455119, and an

brightness increase over

minutes on JD 2454816; in the R band, an

brightness increase over

minutes on JD 2454004, and an

brightness increase over

minutes on JD 2453995; and in the I band, an

brightness decrease over ΔT = 38.44 minutes on JD 2453995, and an

brightness decrease over ΔT = 344.02 minutes on JD 2454818. For micro-variability, we found that R variability leads I variability by 25.92 ± 1.09 minutes. When the periodicity analysis methods, with the red noise being considered, are adopted to the V, R, and I observations, we can find that the periodogram to the V data is consistent with red noise, except for 1 CLEANest peak corresponding to the timescale of 696.0 ± 182.0 days, those to the R data are 653.0 ± 171.0 and 156.0 ± 17.0 days; and those to the I data are 801.0 ± 207.0 and 156.0 ± 15.0 days, respectively.
The California-Kepler Survey. IV. Metal-rich Stars Host a Greater Diversity of Planets
Authors: Petigura Erik A. , Marcy Geoffrey W. , Winn Joshua N. , Weiss Lauren M. , Fulton Benjamin J. , Howard Andrew W. , Sinukoff Evan , Isaacson Howard , Morton Timothy D. , Johnson John Asher 
Published: January 2018

Abstract
Probing the connection between a star’s metallicity and the presence and properties of any associated planets offers an observational link between conditions during the epoch of planet formation and mature planetary systems. We explore this connection by analyzing the metallicities of Kepler target stars and the subset of stars found to host transiting planets. After correcting for survey incompleteness, we measure planet occurrence: the number of planets per 100 stars with a given metallicity M. Planet occurrence correlates with metallicity for some, but not all, planet sizes and orbital periods. For warm super-Earths having P = 10–100 days and

= 1.0–1.7

, planet occurrence is nearly constant over metallicities spanning −0.4 to +0.4 dex. We find 20 warm super-Earths per 100 stars, regardless of metallicity. In contrast, the occurrence of warm sub-Neptunes (

= 1.7–4.0

) doubles over that same metallicity interval, from 20 to 40 planets per 100 stars. We model the distribution of planets as

, where β characterizes the strength of any metallicity correlation. This correlation steepens with decreasing orbital period and increasing planet size. For warm super-Earths β =

, while for hot Jupiters β =

. High metallicities in protoplanetary disks may increase the mass of the largest rocky cores or the speed at which they are assembled, enhancing the production of planets larger than 1.7

. The association between high metallicity and short-period planets may reflect disk density profiles that facilitate the inward migration of solids or higher rates of planet–planet scattering.
A Testable Conspiracy: Simulating Baryonic Effects on Self-interacting Dark Matter Halos
Authors: Elbert Oliver D. , Bullock James S. , Kaplinghat Manoj , Garrison-Kimmel Shea , Graus Andrew S. , Rocha Miguel 
Published: January 2018

Abstract
We investigate the response of self-interacting dark matter (SIDM) halos to the growth of galaxy potentials using idealized simulations, with each run in tandem with collisionless cold dark matter (CDM). We find that if the stellar potential strongly dominates in the central parts of a galaxy, then SIDM halos can be as dense as CDM halos on observable scales. For extreme cases, core collapse can occur, leading to SIDM halos that are denser and cuspier than their CDM counterparts. If the stellar potential is not dominant, then SIDM halos retain isothermal cores with densities far below CDM predictions. When a disk is present, the inner SIDM halo becomes more flattened in the disk plane than the CDM halo. These results are in excellent quantitative agreement with the predictions of Kaplinghat et al. We also simulated a cluster halo with a central stellar distribution similar to the brightest central galaxy of the cluster A2667. An SIDM halo simulated with the cross-section over mass

provides a good match to the measured dark matter (DM) density profile, while an adiabatically contracted CDM halo is denser and cuspier. The profile of the same halo simulated with

is not dense enough. Our findings are in agreement with previous results that

is disfavored for DM collision velocities above about 1500 km s−1. More generally, the interaction between baryonic potentials and SIDM densities offers new directions for constraining SIDM cross-sections in galaxies where baryons are dynamically important.
Clumpy Galaxies in CANDELS. II. Physical Properties of UV-bright Clumps at 0.5 ≤ z < 3
Authors: Guo Yicheng , Rafelski Marc , Bell Eric F. , Conselice Christopher J. , Dekel Avishai , Faber S. M. , Giavalisco Mauro , Koekemoer Anton M. , Koo David C. , Lu Yu , Mandelker Nir , Primack Joel R. , Ceverino Daniel , de Mello Duilia F. , Ferguson Henry C. , Hathi Nimish , Kocevski Dale , Lucas Ray A. , Pérez-González Pablo G. , Ravindranath Swara , Soto Emmaris , Straughn Amber , Wang Weichen 
Published: January 2018

Abstract
Studying giant star-forming clumps in distant galaxies is important to understand galaxy formation and evolution. At present, however, observers and theorists have not reached a consensus on whether the observed “clumps” in distant galaxies are the same phenomenon that is seen in simulations. In this paper, as a step to establish a benchmark of direct comparisons between observations and theories, we publish a sample of clumps constructed to represent the commonly observed “clumps” in the literature. This sample contains 3193 clumps detected from 1270 galaxies at

0.5
≤
z
<
3.0

. The clumps are detected from rest-frame UV images, as described in our previous paper. Their physical properties (e.g., rest-frame color, stellar mass (

M

*

), star formation rate (SFR), age, and dust extinction) are measured by fitting the spectral energy distribution (SED) to synthetic stellar population models. We carefully test the procedures of measuring clump properties, especially the method of subtracting background fluxes from the diffuse component of galaxies. With our fiducial background subtraction, we find a radial clump U − V color variation, where clumps close to galactic centers are redder than those in outskirts. The slope of the color gradient (clump color as a function of their galactocentric distance scaled by the semimajor axis of galaxies) changes with redshift and

M

*

of the host galaxies: at a fixed

M

*

, the slope becomes steeper toward low redshift, and at a fixed redshift, it becomes slightly steeper with

M

*

. Based on our SED fitting, this observed color gradient can be explained by a combination of a negative age gradient, a negative E(B − V) gradient, and a positive specific SFR gradient of the clumps. We also find that the color gradients of clumps are steeper than those of intra-clump regions. Correspondingly, the radial gradients of the derived physical properties of clumps are different from those of the diffuse component or intra-clump regions.
A Model of Titan-like Chemistry to Connect Experiments and Cassini Observations
Authors: Raymond Alexander W. , Sciamma-O’Brien Ella , Salama Farid , Mazur Eric 
Published: January 2018

Abstract
A numerical model is presented for interpreting the chemical pathways that lead to the experimental mass spectra acquired in the Titan Haze Simulation (THS) laboratory experiments and for comparing the electron density and temperature of the THS plasma to observations made at Titan by the Cassini spacecraft. The THS plasma is a pulsed glow-discharge experiment designed to simulate the reaction of N2/CH4-dominated gas in Titan's upper atmosphere. The transient, one-dimensional model of THS chemistry tracks the evolution of more than 120 species in the direction of the plasma flow. As the minor species C2H2 and C2H4 are added to the N2/CH4-based mixture, the model correctly predicts the emergence of reaction products with up to five carbon atoms in relative abundances that agree well with measured mass spectra. Chemical growth in Titan's upper atmosphere transpires through ion–neutral and neutral–neutral chemistry, and the main reactions involving a series of known atmospheric species are retrieved from the calculation. The model indicates that the electron density and chemistry are steady during more than 99% of the 300 μs long discharge pulse. The model also suggests that the THS ionization fraction and electron temperature are comparable to those measured in Titan's upper atmosphere. These findings reaffirm that the THS plasma is a controlled analog environment for studying the first and intermediate steps of chemistry in Titan's upper atmosphere.
A Hydrodynamic Model of Alfvénic Wave Heating in a Coronal Loop and Its Chromospheric Footpoints
Authors: Reep Jeffrey W. , Russell Alexander J. B. , Tarr Lucas A. , Leake James E. 
Published: January 2018

Abstract
Alfvénic waves have been proposed as an important energy transport mechanism in coronal loops, capable of delivering energy to both the corona and chromosphere and giving rise to many observed features of flaring and quiescent regions. In previous work, we established that resistive dissipation of waves (ambipolar diffusion) can drive strong chromospheric heating and evaporation, capable of producing flaring signatures. However, that model was based on a simplified assumption that the waves propagate instantly to the chromosphere, an assumption that the current work removes. Via a ray-tracing method, we have implemented traveling waves in a field-aligned hydrodynamic simulation that dissipate locally as they propagate along the field line. We compare this method to and validate against the magnetohydrodynamics code Lare3D. We then examine the importance of travel times to the dynamics of the loop evolution, finding that (1) the ionization level of the plasma plays a critical role in determining the location and rate at which waves dissipate; (2) long duration waves effectively bore a hole into the chromosphere, allowing subsequent waves to penetrate deeper than previously expected, unlike an electron beam whose energy deposition rises in height as evaporation reduces the mean-free paths of the electrons; and (3) the dissipation of these waves drives a pressure front that propagates to deeper depths, unlike energy deposition by an electron beam.
VLBA Determination of the Distance to Nearby Star-forming Regions. VIII. The LkHα 101 Cluster
Authors: Dzib Sergio A. , Ortiz-León Gisela N. , Loinard L. , Mioduszewski A. J. , Rodríguez L. F. , Medina S.-N. X. , Torres R. M. 
Published: January 2018

Abstract
The LkHα 101 cluster takes its name from its more massive member, the LkHα 101 star, which is an ∼15 M
⊙ star whose true nature is still unknown. The distance to the LkHα 101 cluster has been controversial for the last few decades, with estimated values ranging from 160 to 800 pc. We have observed members and candidate members of the LkHα 101 cluster with signs of magnetic activity, using the Very Long Baseline Array, in order to measure their trigonometric parallax and, thus, obtain a direct measurement of their distances. A young star member, LkHα 101 VLA J043001.15+351724.6, was detected at four epochs as a single radio source. The best fit to its displacement on the plane of the sky yields a distance of 535 ± 29 pc. We argue that this is the distance to the LkHα 101 cluster.
A Self-consistent Model of the Solar Tachocline
Authors: Wood T. S. , Brummell N. H. 
Published: January 2018

Abstract
We present a local but fully nonlinear model of the solar tachocline, using three-dimensional direct numerical simulations. The tachocline forms naturally as a statistically steady balance between Coriolis, pressure, buoyancy, and Lorentz forces beneath a turbulent convection zone. Uniform rotation is maintained in the radiation zone by a primordial magnetic field, which is confined by meridional flows in the tachocline and convection zone. Such balanced dynamics has previously been found in idealized laminar models, but never in fully self-consistent numerical simulations.
The Outcome of HIV-Positive Late Presenters According to Detectable CMV DNA and Anti-CMV Treatment
Authors: Bigliano Paolo , Calcagno Andrea , Lucchini Anna , Audagnotto Sabrina , Montrucchio Chiara , Marinaro Letizia , Alcantarini Chiara , Ghisetti Valeria , Perri Giovanni Di , Bonora Stefano 
Published: January 2018

Background HIV late presenters are at high risk of cytomegalovirus (CMV) reactivation and end-organ disease. CMV viraemia has been associated with poor survival but the effect of anti-CMV treatment has not been studied in this setting. Methods HIV-positive patients were included in a retrospective study if presenting with <350 CD4+ T-cells/μl and starting an antiretroviral treatment within 3 months of the diagnosis. Primary end point was 5-year survival according to the presence of CMV viraemia, CMV end-organ disease and anti-CMV treatment. Results 302 patients were included. 157 patients (52%) presented CMV viraemia (CMV-V) and 44 (14.6%) CMV end-organ disease (CMV-EOD). 5-year mortality was higher in CMV-EOD and CMV-V patients than in CMV-negative patients (11.4 versus 9.6 versus 0%; P=0.002). In patients with CMV-V, 5-year mortality was numerically higher in untreated patients (12.9% versus 6.9%; P=0.257) without reaching statistical significance. At univariate analysis the diagnosis of serious opportunistic infections (cryptococcosis, progressive multifocal leukoencephalopathy, lymphoma; P=0.001) and the absence of a negative CMV DNA in the follow-up ( P<0.001) were associated with poor outcome. At multivariate analysis HCV coinfection ( P=0.016; aOR 6.98, 95% CI 1.50, 32.59), the absence of a negative CMV DNA in the follow-up ( P<0.001; aOR 19.40, 95% CI 3.70, 101.64) and marginally the absence of anti-CMV treatment ( P=0.052; aOR 4.944, 95% CI 0.99, 24.73) were independent predictors of poor outcome. Conclusions CMV reactivation in HIV-positive patients with poor immunity is associated with worse prognosis: the pre-emptive use of anti-CMV therapy was associated with a better outcome in patients with CMV-V.