bluuebunny/crossref_metadata_2025_split huggingface dataset:
LEARNER AUTONOMY ON ESSAY WRITING ACCURACY
Authors: Hafidz Moh. 
Published: February 2018

Abstract: Learner autonomy on writing is independently teaching and learning that keeps students’ control to explore their knowledge and experiences in written language, find out and evaluate their errors based on the conceptual courses to make accurately simple essay. The aim was to know the effectiveness of the learner autonomy on writing accuracy. This quantitative research conducted in one group pretest and posttest design. The number of samples was 21 students in Bangkalan. The instrument were tests to gain students’ writing score before and after treatment. Researcher statistically analyzed the data using SPSS 23 version by running a Paired Samples Test. The result shown the means of pretes score was 66,83 and posttest score was 74,57, Paired Samples Correlations was 0,614 (strong correlation). Significance was 0,005, it means that a (0,05) is higher than r value (0,005) with high variance of mean value (14,091). As a result, the hypothesis (H1­) was received that learner autonomy contributed effectively to learners’ in organizing own ideas (Ene, 2006) such as making a topic map becomes some explanable sub-topics, writing down main and supporting idea, clustering some objects, editing next and learners absolutely accumulate some selected vocabularies inappropriate topics (Chengping W, 2008).Keyword: Learner Autonomy, Learning process, outcomesAbsrak: Pembelajaran otonomi adalah pembelajaran mandiri yang mengontrol mahasiswa untuk menyampaikan gagasan dan pengalamannya, mencatat dan mengevaluasi kesalahan yang terjadi dalam penulisan esai sederhana berdasarkan pembelajaran yang tersetruktur. Tujuan adalah untuk mengetahui efektifitas pembelajaran otonomi terhadap akurasi tulisan secara statistik. Penelitian ini dilakukan dengan menggunakan desain tes awal dan akhir. Jumlah sampel terdiri dari 21 siswa di Bangkalan. Isntrumen yang digunakan adalah tes untuk mengetahui hasil nilai mahasiswa sebelum dan sesudah melakukan pembelajaran otonomi. Peneliti menganalisa data dengan menggunakan versi SPSS 23 dengan menggunakan sampel tes yang berpasangan. Hasil rata-rata tes awal adalah 66,83 dan tes akhir adalah 74,57, dengan corelasi sampel berpasangannya adalah 0,614 (kuat). Sedangkan signifikansinya adalah 0,005, artinya a (0,05) lebih besar daripada r value (0,005) dengan varian nilai rata-rata yang tinggi (14,091). Hasil hipotesis (H1)-nya diterima bahwa pembelajara otonomi berkontribusi secara efektif terhadap pengorganisasian gagasan mahasiswa sendiri (Ene, 2006) seperti memetakan suatu topik menjadi sub-topik yang mudah dijelaskan, pengelompokan objek tertentu untuk dijadikan topik, kemudian mengeditnya dan tentunya dapat memilih kosakat-kosakata yang sesuai dengan topiknya (Chengping W, 2008).Kata Kunci: pemanfaatan media, pembelajaran sains
PEMANFAATAN MEDIA VIDEO UNTUK MENINGKATKAN HASIL BELAJAR PRAKTIK BERWUDHLU KELAS 2 SDN PRAMBON MADIUN
Authors: Insiyah Insiyah , Fadhli Muhibuddin 
Published: February 2018

Abstract: Instructional media is one of the important components in the learning process. Utilization can be very crucial in the learning process. Video is one type of audio-based learning media. One of the advantages of this media is that it can be rotated anytime and anywhere, so that students can independently utilize the media. The purpose of this research is to improve the learning result of the ablution practice which in practice there are still many mistakes. This study is action class research with two cycles. With minimum completeness criteria (KKM) 80 where the result of the first cycle of KKM students get an average of 75 and in the second cycle the average student learning outcomes score 85.Keywords: Video, Learning Result, Ablution. Abstrak: Media pembelajaran adalah salah satu komponen penting dalam proses pembelajaran. Pemanfaatannya bisa menjadi sangat krusial dalam proses pembelajaran. Media video adalah salah satu jenis media pembelajaran berbasis audio visual. Salah satu keunggulan media ini adalah dapat diputar kapan dan dimana saja, sehingga siswa dapat secara mandiri memanfaatkan media tersebut. Tujuan dari penelitian ini adalah untuk meningkatkan hasil belajar praktik berwudhlu yang dalam praktiknya masih banyak ditemui banyak kesalahan. Penelitian ini adalah peneltian tindakan kelas dengan dua siklus. Dengan KKM 80 dimana hasil dari siklus pertama KKM siswa memperoleh rata-rata 75 dan pada siklus kedua rata-rata hasil belajar siswa memperoleh nilai 85.Kata Kunci: Video, Hasil belajar, Berwudhu.
Peripheral nerve grafts implanted into the substantia nigra in patients with Parkinson’s disease during deep brain stimulation surgery: 1-year follow-up study of safety, feasibility, and clinical outcome
Authors: van Horne Craig G. , Quintero Jorge E. , Slevin John T. , Anderson-Mooney Amelia , Gurwell Julie A. , Welleford Andrew S. , Lamm John R. , Wagner Renee P. , Gerhardt Greg A. 
Published: February 2018

OBJECTIVECurrently, there is no treatment that slows or halts the progression of Parkinson’s disease. Delivery of various neurotrophic factors to restore dopaminergic function has become a focus of study in an effort to fill this unmet need for patients with Parkinson’s disease. Schwann cells provide a readily available source of such factors. This study presents a 12-month evaluation of safety and feasibility, as well as the clinical response, of implanting autologous peripheral nerve grafts into the substantia nigra of patients with Parkinson’s disease at the time of deep brain stimulation (DBS) surgery.METHODSStandard DBS surgery targeting the subthalamic nucleus was performed in 8 study participants. After DBS lead implantation, a section of the sural nerve containing Schwann cells was harvested and unilaterally grafted to the substantia nigra. Adverse events were continually monitored. Baseline clinical data were obtained during standard preoperative evaluations. Clinical outcome data were obtained with postoperative clinical evaluations, neuropsychological testing, and MRI at 1 year after surgery.RESULTSAll 8 participants were implanted with DBS systems and grafts. Adverse event profiles were comparable to those of standard DBS surgery with the exception of 1 superficial infection at the sural nerve harvest site. Three participants also reported numbness in the distribution of the sural nerve distal to the harvest site. Motor scores on Unified Parkinson’s Disease Rating Scale (UPDRS) part III while the participant was off therapy at 12 months improved from baseline (mean ± SD 25.1 ± 15.9 points at 12 months vs 32.5 ± 9.7 points at baseline). An analysis of the lateralized UPDRS scores also showed a greater overall reduction in scores on the side contralateral to the graft.CONCLUSIONSPeripheral nerve graft delivery to the substantia nigra at the time of DBS surgery is feasible and safe based on the results of this initial pilot study. Clinical outcome data from this phase I trial suggests that grafting may have some clinical benefit and certainly warrants further study to determine if this is an efficacious and neurorestorative therapy.Clinical trial registration no.: NCT01833364 (clinicaltrials.gov)
Safe insertion of S-2 alar iliac screws: radiological comparison between 2 insertion points using computed tomography and 3D analysis software
Authors: Yamada Kentaro , Abe Yuichiro , Satoh Shigenobu 
Published: February 2018

OBJECTIVES-2 alar iliac (S2AI) screws are commonly used as anchors for lumbosacral fixation. A serious potential complication of screw insertion is major vascular injury due to anterior or caudal screw deviation. To avoid screw deviation, the pelvic inlet view on intraoperative fluoroscopy images is recommended. However, there has been no detailed investigation of optimal fluoroscopic incline with the pelvic inlet view. The purpose of this study was to investigate the safety margins and to optimize fluoroscopic settings to avoid screw deviation with 2 reported insertion techniques using 3D analysis software and CT.METHODSThe study included 50 patients (25 men and 25 women) who underwent abdominal-pelvic CT. With the use of software, the ideal S2AI screws were set from 2 entry points: A) the midpoint between the S-1 dorsal foramen and the S-2 dorsal foramen where they meet the lateral sacral crest, and B) 1 mm inferior and 1 mm lateral to the S-1 dorsal foramen. Anteriorly or caudally deviated screws were defined as deviation of a half thread of the ideal screw by rotation anteriorly or caudally from the entry point. The angular safety margins were compared between the 2 entry points, and patients with small safety margins were investigated. Subsequently, fluoroscopic images were virtualized on ray sum–rendered images. Conditions that provided proper recognition of screw deviation were investigated via lateral and anteroposterior views with the beam tilted caudally.RESULTSThe safety margins of S2AI screws were smaller in the anterior direction than in the caudal direction and by entry point A than by entry point B (A: 9.1° ± 1.6° and B: 9.7° ± 1.5° in the anterior direction; A: 10.9° ± 3.8° and B: 13.9° ± 4.1° in the caudal direction). In contrast, patients with a deep-seated L-5 vertebral body tended to have smaller safety margins in the caudal direction. All anteriorly deviated screws were recognized with a 60°–70° inlet view from the S-1 slope. The caudally deviated screws were all recognized on the lateral view, but 31% of screws at entry point A and 21% of screws at entry point B were not recognized on the pelvic inlet view.CONCLUSIONSS2AI screws should be carefully placed to avoid anterior deviation compared with caudal deviation in terms of the safety margin, except in patients with a deep-seated L-5. The difference in safety margins between entry points A and B was negligible. Intraoperative fluoroscopy is recommended with a pelvic inlet view tilted 60°–70° from the S-1 slope to avoid anterior screw deviation. The lateral view is recommended to confirm that the screw is not deviated caudally.
Differential distribution patterns in cerebellar irrigation. A study with autopsy material
Authors: Estupiñan Hernando Yesid , Gomez Fabian Alejandro , Ballesteros Luis Ernesto 
Published: February 2018

Aim: The aim of this investigation was characterize morphologically the cerebellar artery and its branches in a specimen of autopsy material.
Methods: This descriptive cross-sectional study evaluated the anatomical characteristics of the cerebellar arteries and their branches in 93 brain stem and cerebellum blocks obtained from fresh cadavers. The specimens were perfused bilaterally channeling the proximal segments of the internal carotid and vertebral arteries with a semi-synthetic resin (Palatal GP40L 85%; styrene 15%) impregnated with mineral red dye. We evaluated the distribution patterns of the cerebellar artery and its branches.
Results: The calibers of the superior cerebellar artery (SCA), anterior inferior cerebellar artery (AICA) and posterior inferior cerebellar artery (PICA) were 1.46 ± 0.2 mm, 1.02 ± 0.35 mm and 1.45 ± 0.37 mm, respectively. Agenesis of the SCA was observed in six specimens (3.2%), AICA in 30 (16.1%), and PICA in 14 (7.5%) specimens. Usual irrigation was observed in 44 (47.3%) cerebellar blocks, whereas 49 (52.7%) specimens showed irrigation variants, 23 (46.9%) of which appeared bilaterally. The dominant distribution of the cerebellar arteries corresponded to SCA in 9 (12.5%) cases, AICA in 46 (63.9%) and PICA in 7 (9.7%) specimens; shared dominance was found in 10 (13.9%) specimens.
Conclusion: The high variability of the cerebellar arteries observed in the present study is consistent with previous reports. The diverse anatomic expressions of the cerebellar arteries were typified in relation to their dominance and territories irrigated, useful for the diagnosis and clinical-surgical management of the cerebellum blood supply.
Transport of Internetwork Magnetic Flux Elements in the Solar Photosphere
Authors: Agrawal Piyush , Rast Mark P. , Gos̆ić Milan , Bellot Rubio Luis R. , Rempel Matthias 
Published: February 2018

Abstract
The motions of small-scale magnetic flux elements in the solar photosphere can provide some measure of the Lagrangian properties of the convective flow. Measurements of these motions have been critical in estimating the turbulent diffusion coefficient in flux-transport dynamo models and in determining the Alfvén wave excitation spectrum for coronal heating models. We examine the motions of internetwork flux elements in Hinode/Narrowband Filter Imager magnetograms and study the scaling of their mean squared displacement and the shape of their displacement probability distribution as a function of time. We find that the mean squared displacement scales super-diffusively with a slope of about 1.48. Super-diffusive scaling has been observed in other studies for temporal increments as small as 5 s, increments over which ballistic scaling would be expected. Using high-cadence MURaM simulations, we show that the observed super-diffusive scaling at short increments is a consequence of random changes in barycenter positions due to flux evolution. We also find that for long temporal increments, beyond granular lifetimes, the observed displacement distribution deviates from that expected for a diffusive process, evolving from Rayleigh to Gaussian. This change in distribution can be modeled analytically by accounting for supergranular advection along with granular motions. These results complicate the interpretation of magnetic element motions as strictly advective or diffusive on short and long timescales and suggest that measurements of magnetic element motions must be used with caution in turbulent diffusion or wave excitation models. We propose that passive tracer motions in measured photospheric flows may yield more robust transport statistics.
Near-infrared Stellar Populations in the Metal-poor, Dwarf Irregular Galaxies Sextans A and Leo A
Authors: Jones Olivia C. , Maclay Matthew T. , Boyer Martha L. , Meixner Margaret , McDonald Iain , Meskhidze Helen 
Published: February 2018

Abstract
We present JHK

s
observations of the metal-poor ([Fe/H] < −1.40) dwarf-irregular galaxies, Leo A and Sextans A, obtained with the WIYN High-resolution Infrared Camera at Kitt Peak. Their near-IR stellar populations are characterized by using a combination of color–magnitude diagrams and by identifying long-period variable stars. We detected red giant and asymptotic giant branch stars, consistent with membership of the galaxy’s intermediate-age populations (2–8 Gyr old). Matching our data to broadband optical and mid-IR photometry, we determine luminosities, temperatures, and dust-production rates (DPR) for each star. We identify 32 stars in Leo A and 101 stars in Sextans A with a DPR

, confirming that metal-poor stars can form substantial amounts of dust. We also find tentative evidence for oxygen-rich dust formation at low metallicity, contradicting previous models that suggest oxygen-rich dust production is inhibited in metal-poor environments. The total rates of dust injection into the interstellar medium of Leo A and Sextans A are

and

, respectively. The majority of this dust is produced by a few very dusty evolved stars and does not vary strongly with metallicity.
Polycyclic Aromatic Hydrocarbons with Straight Edges and the 7.6/6.2 and 8.6/6.2 Intensity Ratios in Reflection Nebulae
Authors: Ricca Alessandra , Bauschlicher Charles W. , Roser Joseph E. , Peeters Els 
Published: February 2018

Abstract
Using density functional theory, we have investigated the mid-infrared spectral characteristics of a series of polycyclic aromatic hydrocarbons (PAHs) that have straight edges and that contain an even or odd number of carbons. For several even and odd-carbon PAHs, the 8.6/6.2 and 7.6/6.2 intensity ratios computed in emission after the absorption of a 8 eV photon match the observed ratios obtained for three reflection nebulae (RNe), namely NGC 1333, NGC 7023, and NGC 2023. Odd-carbon PAHs are favored, particularly for NGC 1333. Both cations and anions are present, with the cations being predominant. Relevant PAHs span sizes ranging from 46 to 113 carbons for NGC 7023 and NGC 2023 and from 38 to 127 carbons for NGC 1333, and have symmetries ranging from D2h
to C
s
. Our work suggests that even- and odd-carbon PAHs with straight edges are viable candidates for the PAH emission seen toward irradiated photodissociation regions.
On the Diversity in Mass and Orbital Radius of Giant Planets Formed via Disk Instability
Authors: Müller Simon , Helled Ravit , Mayer Lucio 
Published: February 2018

Abstract
We present a semi-analytical population synthesis model of protoplanetary clumps formed by disk instability at radial distances of 80–120 au. Various clump density profiles, initial mass functions, protoplanetary disk models, stellar masses, and gap opening criteria are considered. When we use more realistic gap opening criteria, we find that gaps open only rarely, which strongly affects clump survival rates and their physical properties (mass, radius, and radial distance). The inferred surviving population is then shifted toward less massive clumps at smaller radial distances. We also find that populations of surviving clumps are very sensitive to the model assumptions and used parameters. Depending on the chosen parameters, the protoplanets occupy a mass range between 0.01 and 16 M
J and may either orbit close to the central star or as far out as 75 au, with a sweet spot at 10–30 au for the massive ones. However, in all of the cases we consider, we find that massive giant planets at very large radial distances are rare, in qualitative agreement with current direct imaging surveys. We conclude that caution should be taken in deriving population synthesis models as well as when comparing the models’ results with observations.
The Physical Characteristics of Interstellar Medium in NGC 3665 with Herschel Observations*
Authors: Xiao Meng-Yuan , Zhao 赵 Yinghe 应和 , Gu Qiu-Sheng , Shi Yong 
Published: February 2018

Abstract
We present the analysis of the physical properties of the interstellar medium in the nearby early-type galaxy NGC 3665, based on the far-infrared photometric and spectroscopic data as observed by the Herschel Space Observatory. The fit to the spectral energy distribution reveals a high dust content in the galaxy, with a dust-to-stellar mass ratio of

/M
* ∼ 1.1 × 10−4 that is nearly three times larger than the mean value of local S0+S0a galaxies. For the ionized regions (H ii regions), the electron density (n

e
) is around 49.5 ± 11.9 cm−3 based on the [N ii] 122 μm/[N ii] 205 μm ratio. For the photodissociation regions, the heating efficiency ranges from 1.26 × 10−3 to 1.37 × 10−3 based on the ([C ii]+[O i] 63 μm)/

, which is slightly lower than other local galaxies; the hydrogen nucleus density and the strength of the far-UV radiation field are n ∼ 104 cm−3 and G
0 ∼ 10−0.25, respectively. The above results are consistent with the presence of weak active galactic nuclei and a low level of star-forming activity in NGC 3665. Our results give strong support to the “morphological quenching” scenario, where a compact, massive bulge can stabilize the amount of cool gas against star formation.
Dusty Cloud Acceleration by Radiation Pressure in Rapidly Star-forming Galaxies
Authors: Zhang Dong , Davis Shane W. , Jiang Yan-Fei , Stone James M. 
Published: February 2018

Abstract
We perform two-dimensional and three-dimensional radiation hydrodynamic simulations to study cold clouds accelerated by radiation pressure on dust in the environment of rapidly star-forming galaxies dominated by infrared flux. We utilize the reduced speed of light approximation to solve the frequency-averaged, time-dependent radiative transfer equation. We find that radiation pressure is capable of accelerating the clouds to hundreds of kilometers per second while remaining dense and cold, consistent with observations. We compare these results to simulations where acceleration is provided by entrainment in a hot wind, where the momentum injection of the hot flow is comparable to the momentum in the radiation field. We find that the survival time of the cloud accelerated by the radiation field is significantly longer than that of a cloud entrained in a hot outflow. We show that the dynamics of the irradiated cloud depends on the initial optical depth, temperature of the cloud, and intensity of the flux. Additionally, gas pressure from the background may limit cloud acceleration if the density ratio between the cloud and background is

. In general, a 10 pc-scale optically thin cloud forms a pancake structure elongated perpendicular to the direction of motion, while optically thick clouds form a filamentary structure elongated parallel to the direction of motion. The details of accelerated cloud morphology and geometry can also be affected by other factors, such as the cloud lengthscale, reduced speed of light approximation, spatial resolution, initial cloud structure, and dimensionality of the run, but these have relatively little affect on the cloud velocity or survival time.
Continuum Reverberation Mapping of the Accretion Disks in Two Seyfert 1 Galaxies
Authors: Fausnaugh M. M. , Starkey D. A. , Horne Keith , Kochanek C. S. , Peterson B. M. , Bentz M. C. , Denney K. D. , Grier C. J. , Grupe D. , Pogge R. W. , De Rosa G. , Adams S. M. , Barth A. J. , Beatty Thomas G. , Bhattacharjee A. , Borman G. A. , Boroson T. A. , Bottorff M. C. , Brown Jacob E. , Brown Jonathan S. , Brotherton M. S. , Coker C. T. , Crawford S. M. , Croxall K. V. , Eftekharzadeh Sarah , Eracleous Michael , Joner M. D. , Henderson C. B. , Holoien T. W.-S. , Hutchison T. , Kaspi Shai , Kim S. , King Anthea L. , Li Miao , Lochhaas Cassandra , Ma Zhiyuan , MacInnis F. , Manne-Nicholas E. R. , Mason M. , Montuori Carmen , Mosquera Ana , Mudd Dale , Musso R. , Nazarov S. V. , Nguyen M. L. , Okhmat D. N. , Onken Christopher A. , Ou-Yang B. , Pancoast A. , Pei L. , Penny Matthew T. , Poleski Radosław , Rafter Stephen , Romero-Colmenero E. , Runnoe Jessie , Sand David J. , Schimoia Jaderson S. , Sergeev S. G. , Shappee B. J. , Simonian Gregory V. , Somers Garrett , Spencer M. , Stevens Daniel J. , Tayar Jamie , Treu T. , Valenti Stefano , Van Saders J. , Villanueva S. , Villforth C. , Weiss Yaniv , Winkler H. , Zhu W. 
Published: February 2018

Abstract
We present optical continuum lags for two Seyfert 1 galaxies, MCG+08-11-011 and NGC 2617, using monitoring data from a reverberation mapping campaign carried out in 2014. Our light curves span the ugriz filters over four months, with median cadences of 1.0 and 0.6 days for MCG+08-11-011 and NGC 2617, respectively, combined with roughly daily X-ray and near-UV data from Swift for NGC 2617. We find lags consistent with geometrically thin accretion-disk models that predict a lag-wavelength relation of τ ∝ λ
4/3. However, the observed lags are larger than predictions based on standard thin-disk theory by factors of 3.3 for MCG+08-11-011 and 2.3 for NGC 2617. These differences can be explained if the mass accretion rates are larger than inferred from the optical luminosity by a factor of 4.3 in MCG+08-11-011 and a factor of 1.3 in NGC 2617, although uncertainty in the SMBH masses determines the significance of this result. While the X-ray variability in NGC 2617 precedes the UV/optical variability, the long (2.6 day) lag is problematic for coronal reprocessing models.