bluuebunny/crossref_metadata_2025_split huggingface dataset:
Prophylaxis of incisional hernia after subcostal laparotomy in hepatobiliar surgery
Authors: Bellido Luque A 
Published: February 2021

Resumen

Introducción: la hernia incisional (HI) es una de las complicaciones más comunes en la cirugía abierta abdominal. Se denomina HI a una solución de continuidad en la fascia abdominal que se manifiesta como una protrusión del contenido intraabdominal a través de dicho defecto, localizado en una incisión practicada previamente en la pared abdominal.

La incidencia de la HI se sitúa en torno al 5-20%, pudiendo llegar al 30% en pacientes con factores de riesgo.

Prevención de la HI en cirugía hepatobiliopancreática (HBP): en relación a las laparotomías medias los estándares de actuación están bien definidos hoy por hoy y se resumen en las guías clínicas. Sin embargo, en las laparotomías más frecuentemente utilizadas en la cirugía hepatobiliar y pancreática, las recomendaciones no son tan claras, aunque parece que la tendencia es generalizar los principios utilizados en las laparotomías medias.
Advances in laparoscopic hernia repair (from IPOM to LIRA)
Authors: Gómez Menchero J , Suárez Grau JM , Fernández Carazo A , Morales Conde S 
Published: February 2021

Resumen

Las actuales tendencias de tratamiento de la hernia ventral por vía laparoscópica apuestan por la reconstrucción mínimamente invasiva de la pared. La necesidad de buscar soluciones a la tasa de bulging o de seroma presentes en el IPOM clásico han sido el objetivo de nuevas técnicas como el cierre del defecto que tratan de restablecer anatómicamente la pared abdominal. Tras diez años de cierre del defecto hemos podido comprobar que existen problemas inherentes a la tensión que genera el cierre del defecto, y que existen factores individuales del paciente y de la hernia a tratar que podrían influir negativamente en la recidiva o el bulging por fallo del cierre del defecto.

El desarrollo de una nueva técnica por parte de nuestro grupo (técnica LIRA), nos ha permitido mejorar la fiabilidad de la reconstrucción de la línea media a largo plazo, fundamentalmente en aquellos pacientes con factores de riesgo, garantizando una reconstrucción duradera en aquellos pacientes con hernias de tamaño medio no subsidiarias de técnicas más complejas como una separación de componentes.
The role of the splenic embolization in blunt spleen trauma.
Authors: Alcaide Lucena M , Martínez Domínguez AP , González Puga C , Mirón Pozo B 
Published: February 2021

Resumen

Objetivo: describir el caso de un varón que presenta traumatismo abdominal cerrado con lesión esplénica.

Material y métodos: paciente de 22 años estable hemodinamicamente tras traumatismo abdominal cerrado, con TAC compatible con lesión esplénica y hemoperitoneo moderado con sangrado activo, tratado mediante embolización arterial.

Resultado: evolución tras embolización favorable. Asintomático al año del evento.

Discusión: clásicamente se han tratado mediante esplenectomía los pacientes con traumatismo esplénico con sangrado activo y hemoperitoneo. Describimos la utilización de esta técnica como método eficaz en pacientes hemodinamicamente estables.

Conclusión: la embolización arterial del bazo es una técnica segura y poco agresiva para el tratamiento de las lesiones traumáticas del bazo en pacientes hemodinamicamente estables con sangrado activo.
Retroperitoneoscopy in acute pancreatitis.
Authors: Tinoco González J , Tallón Aguilar L , Sánchez Arteaga A , Perea del Pozo E , Durán Muñoz-Cruzado V , Díaz Gómez D , Tamayo López MJ , Nevado Infante A , Aparicio Sánchez D , Padillo Ruiz J 
Published: February 2021

Resumen

La pancreatitis aguda es un proceso inflamatorio donde el tratamiento médico precoz y una secuencia de abordaje escalonada (step-up approach) reduce, significativamente, la morbilidad y mortalidad. El desarrollo de la laparoscopia ha permitido disponer de abordajes mínimamente invasivos como la retroperitoneoscopia (VARD).

La VARD es una técnica poco invasiva que minimiza la respuesta sistémica al estrés quirúrgico. Ofrece la ventaja de una mejor visualización de las estructuras vasculares pancreáticas y minimiza la lesión de éstas. Permite realizar nuevos lavados y drenajes por vía retroperitoneal, evitando la altísima morbi-mortalidad asociada a una laparotomía.

La VARD es una técnica quirúrgica alternativa, válida y reproducible en el tratamiento de la PAN, que ofrece resultados comparables e incluso superiores, en algunas series, a los de la cirugía abierta, con resultados satisfactorios en cuanto a morbilidad y mortalidad postoperatoria.
Various Disinfecting Methods of Orthodontic Pliers in Daily Clinical Practice: A comparative Study
Authors: Purva Verma, Arvind Sivkumar  
Published: February 2021

Introduction: Orthodontic pliers are essential armamentarium in every orthodontic office and should be used
once for one patient, then autoclaved before next use. Clinical orthodontics with higher volume of patients,
requires a quick chair side disinfection method for pliers, also in rural centres with minimum infrastructure
it is a challenge to maintain sterilisation protocols. Various disinfecting agents include alcohols , quaternary
ammonium salts, formaldehyde, chloramine, sodium hypochlorite, spirit, glutaraldehyde etc. are available.
Out of these we compared the commonly available disinfectants including ethyl alcohol, 5% glutaraldehyde,
and 6% sodium hypochlorite to assess their disinfection efficacy after clinical use.
Materials and method: 20 orthodontic pliers were inoculated with Coagulase negative streptococci. The
pliers were divided in 4 groups with 5 pliers in each group. Each group was subjected to different disinfectant
solution with one group aiding as control. The disinfectants used were: spirit (group 1), 5% glutaraldehyde
(group 2), 2% sodium hypochlorite (group 3) and distilled water (control group).
Results: spirit and 5% glutaraldehyde have shown to be potent disinfectants.
Conclusions: Based on these results, we concluded that among the tested methods, disinfection of orthodontic
pliers with spirit and 5% glutaraldehyde are the efficient methods for chair-side disinfection.
Акме-орієнтири розвитку представників покоління Z у контексті рефлексивно-проєктної парадигми освіти
Authors: Чумак Л.В.  
Published: February 2021

У статті представлено концептуальні положення теорії поколінь у контексті рефлексивно-проєктної парадигми освіти. Її метою визначено виокремлення способів удосконалення освітнього процесу сучасної молоді в напрямі значущих структурних компонентів означеної парадигми освіти. Завданнями дослідження є висвітлення особливостей цифрового покоління і психолого-педагогічного контексту рефлексивно-проєктної парадигми освіти для можливості трансформації їх у наукове поле методологічного і методичного знання з подальшим практичним відтворенням певних базисних положень. Методологічну основу становлять концептуальні положення теорії поколінь; філософські, психологічні та педагогічні аспекти освіти; акме-теорії розвитку особистості як суб’єкта діяльності з використанням історичного наративу; аналіз і узагальнення одержаної інформації щодо психологічних характеристик «цифрових дітей» та значущих структурних компонентів рефлексивно-проєктної парадигми освіти для можливості подальшого більш чіткого проєктування вектора акме-траєкторії означеного феномена як об’єктивної потреби освітньої практики у модернізації. Дослідження виконано в руслі комплексного поєднання особистісного, системно-структурного та контекстного підходів до розгляду акме-орієнтирів розвитку молоді у контексті рефлексивно-проєктної парадигми освіти. Використано такі методи дослідження: структурно-аналітичний метод і порівняльно-історичний, які дозволяють вивчати спадкоємні зв’язки між різними ідеями; метод систематизації наукових ідей; метод інтерпретації фактологічних даних; метод прогностичного мислення з орієнтацією на прогноз якісного результату. Новизна дослідження полягає у розробці алгоритму реалізації рефлексивно-проєктної парадигми освіти та визначенні її базисних положень як акме-орієнтирів розвитку молоді покоління Z.
Ключові слова: теорія поколінь, соціально-психологічні особливості молоді покоління Z, алгоритм реалізації рефлексивно-проєктної парадигми освіти, базисні положення.
Ground Vibrational State SiO Emission in the VLA BAaDE Survey
Authors: Dike V. , Morris M. R. , Rich R. M. , Lewis M. O. , Quiroga-Nuñez L. H. , Stroh M. C. , Trapp A. C. , Claussen M. J. 
Published: February 2021

Abstract
Using a subsample of the Bulge Asymmetries and Dynamical Evolution (BAaDE) survey of stellar SiO masers, we explore the prevalence and characteristics of 28SiO J = 1 − 0, v = 0 emission. We identify 90 detections of maser, thermal, or composite 28SiO J = 1 − 0, v = 0 emission out of approximately 13,000 candidate spectra from the National Science Foundation’s Karl G. Jansky Very Large Array (VLA). We find that the detected sources are likely asymptotic giant branch stars belonging to a bright, foreground Milky Way stellar disk population. For the 32 sources showing thermal components, we extract values for outflow velocity by fitting thermal line profiles. We find a range of circumstellar envelope expansion velocities, and compare to previously recorded OH and CO expansion velocities. This preliminary survey is already the largest study of stellar ground vibrational state SiO masers to date, and will be expanded to include the entire VLA BAaDE data set when data reduction for the 18,988 target sources is completed.
First Observations of an Ion Vortex in a Magnetic Hole in the Solar Wind by MMS
Authors: Wang G. Q. , Volwerk M. , Wu M. Y. , Hao Y. F. , Xiao S. D. , Wang G. , Liu L. J. , Chen Y. Q. , Zhang T. L. 
Published: February 2021

Abstract
The coronal heating region is able to generate mirror mode structures by ion mirror instabilities. Linear magnetic holes are believed to be the remnants of mirror mode structures, thus they are believed to be messengers from the coronal heating region. They can be convected to ∼9 au with the solar wind flow, indicating that a stabilizing mechanism is necessary to make the magnetic holes survive for such a long time. Here, we investigate a magnetic hole with a size of ∼6.7 ρ
i in the solar wind based on observations by the Magnetospheric Multiscale mission. The unprecedented high-resolution data enable us to reveal the existence of the ion vortex inside the structure for the first time. Such an ion vortex forms a ring-like current, which is consistent with the magnetic field depression. The self-consistent structure of the magnetic hole contributed by the ion vortex can help to further shed light on the mechanism of the long-term survival of magnetic holes in the astrophysical plasma.
NuSTAR Observation of Energy Release in 11 Solar Microflares
Authors: Duncan Jessie , Glesener Lindsay , Grefenstette Brian W. , Vievering Juliana , Hannah Iain G. , Smith David M. , Krucker Säm , White Stephen M. , Hudson Hugh 
Published: February 2021

Abstract
Solar flares are explosive releases of magnetic energy. Hard X-ray (HXR) flare emission originates from both hot (millions of Kelvin) plasma and nonthermal accelerated particles, giving insight into flare energy release. The Nuclear Spectroscopic Telescope ARray (NuSTAR) utilizes direct-focusing optics to attain much higher sensitivity in the HXR range than that of previous indirect imagers. This paper presents 11 NuSTAR microflares from two active regions (AR 12671 on 2017 August 21 and AR 12712 on 2018 May 29). The temporal, spatial, and energetic properties of each are discussed in context with previously published HXR brightenings. They are seen to display several “large flare” properties, such as impulsive time profiles and earlier peak times in higher-energy HXRs. For two events where the active region background could be removed, microflare emission did not display spatial complexity; differing NuSTAR energy ranges had equivalent emission centroids. Finally, spectral fitting showed a high-energy excess over a single thermal model in all events. This excess was consistent with additional higher-temperature plasma volumes in 10/11 microflares and only with an accelerated particle distribution in the last. Previous NuSTAR studies focused on one or a few microflares at a time, making this the first to collectively examine a sizable number of events. Additionally, this paper introduces an observed variation in the NuSTAR gain unique to the extremely low livetime (<1%) regime and establishes a correction method to be used in future NuSTAR solar spectral analysis.
Formation of Massive Star Clusters by Fast H i Gas Collision
Authors: Maeda Ryunosuke , Inoue Tsuyoshi , Fukui Yasuo 
Published: February 2021

Abstract
Young massive clusters (YMCs) are dense aggregates of young stars, which are essential to galaxy evolution, owing to their ultraviolet radiation, stellar winds, and supernovae. The typical mass and radius of YMCs are M ∼ 104
M
⊙ and R ∼ 1 pc, respectively, indicating that many stars are located in a small region. The formation of YMC precursor clouds may be difficult because a very compact massive cloud should be formed before stellar feedback blows off the cloud. Recent observational studies suggest that YMCs can be formed as a consequence of the fast H i gas collision with a velocity of ∼100 km s−1, which is the typical velocity of the galaxy–galaxy interaction. In this study, we examine whether the fast H i gas collision triggers YMC formation using three-dimensional magnetohydrodynamics simulations, which includes the effects of self-gravity, radiative cooling/heating, and chemistry. We demonstrate that massive gravitationally bound gas clumps with M > 104
M
⊙ and L ∼ 4 pc are formed in the shock compressed region induced by the fast H i gas collision, in which massive gas clumps can evolve into YMCs. Our results show that the YMC precursors are formed by the global gravitational collapse of molecular clouds, and YMCs can be formed even in low-metal environments, such as the Magellanic Clouds. Additionally, the very massive YMC precursor cloud, with M > 105
M
⊙, can be created when we consider the fast collision of H i clouds, which may explain the origin of the very massive stellar cluster R136 system in the Large Magellanic Cloud.
Golden Galactic Binaries for LISA: Mass-transferring White Dwarf Black Hole Binaries
Authors: Sberna Laura , Toubiana Alexandre , Miller M. Coleman 
Published: February 2021

Abstract
We study the evolution and gravitational wave emission of white dwarf–black hole accreting binaries with a semianalytical model. These systems will evolve across the mHz gravitational wave frequency band and potentially be detected by the Laser Interferometer Space Antenna (LISA). We identify new universal relations for this class of binaries, which relate the component masses to the gravitational wave frequency and its first derivative. Combined with the high precision measurements possible with LISA, these relations could allow us to infer the component masses and the luminosity distance of the source. LISA has therefore the potential to detect and characterize a virtually unexplored binary population.
Baryonic Feedback Measurement From KV450 Cosmic Shear Analysis
Authors: Yoon Mijin , Jee M. James 
Published: February 2021

Abstract
While baryonic feedback is one of the most important astrophysical systematics that we need to address in order to achieve precision cosmology, few weak lensing studies have directly measured its impact on the matter power spectrum. We report measurement of the baryonic feedback parameter with the constraints on its lower and upper limits from cosmic shear. We use the public data from the Kilo-Degree Survey and the VISTA Kilo-Degree Infrared Galaxy Survey spanning 450 deg2. Estimating both cosmological and feedback parameters simultaneously, we obtain

A

b

=

1.01

−
0.85

+
0.80

, which shows a consistency with the dark matter-only (DMO) case at the ∼1.2σ level and a tendency toward positive feedback; the A
b = 0 (0.81) value corresponds to the DMO (OWLS AGN) case. Despite this full constraint of the feedback parameter, our

S

8

(
≡

σ

8

Ω

m

/

0.3

)

measurement (

0.739

−
0.035

+
0.036

) shifts by only ∼6% of the statistical error, compared to the previous measurement. When we assume the flat ΛCDM cosmology favored by the Nine-Year Wilkinson Microwave Anisotropy Probe (Planck) result, the feedback parameter is constrained to be

A

b

=

1.21

−
0.54

+
0.61

(

1.60

−
0.52

+
0.53

), which excludes the DMO case at the ∼2.2σ (∼3.1σ) level.
Whistlers in the Solar Vicinity That Are Spiky in Time and Frequency
Authors: Mozer F. S. , Bonnell J. W. , Halekas J. S. , Rahmati A. , Schum G. , Vasko I. V. 
Published: February 2021

Abstract
Spiky whistlers are short duration chirps of electric field that have fine structures in both frequency and time. They are observed on the Parker Solar Probe for the first time. From the limited available data, they appear to be accompanied by low-frequency ion waves and to occur relatively frequently. The origin of these wave pairs and their correlations are not understood.
Wave-driven Shocks in Stellar Outbursts: Dynamics, Envelope Heating, and Nascent Blast Waves
Authors: Matzner Christopher D. , Ro Stephen 
Published: February 2021

Abstract
We address the shocks from acoustic pulses and wave trains in general one-dimensional flows, with an emphasis on the application to super-Eddington outbursts in massive stars. Using approximate adiabatic invariants, we generalize the classical equal-area technique in its integral and differential forms. We predict shock evolution for the case of an initially sinusoidal but finite wave train, with separate solutions for internal shocks and head or tail shocks, and demonstrate detailed agreement with numerical simulations. Our internal shock solution motivates improved expressions for the shock-heating rate. Our solution for head and tail shocks demonstrates that these preserve dramatically more wave energy to large radii and have a greater potential for the direct ejection of matter. This difference highlights the importance of the waveform for shock dynamics. Our weak-shock analysis predicts when shocks will become strong and provides a basis from which this transition can be addressed. We use it to estimate the mass ejected by sudden sound pulses and weak central explosions.
Detection of GeV Gamma-ray Emission of Kepler’s SNR With Fermi-LAT
Authors: Xiang Yunchuan , Jiang Zejun 
Published: February 2021

Abstract
A likely detection of γ-ray emission from the region of Kepler’s Supernova Remnant (SNR) is reported by analyzing ∼12 yr of Pass 8 data of the Fermi Large Area Telescope. Its photon flux is (4.85 ± 0.60) × 10−10 ph cm−2 s−1 with ∼4σ significance in 0.2−500 GeV. Moreover, our results show that there is no significant variability in the light curve of ∼12 yr, and its position can well overlap with the observation result of Chandra in hard X-ray band with a good spatial resolution of 0.″5, so the source is likely to be the GeV γ-ray counterpart of Kepler’s SNR. The spectral energy distribution of γ-rays from Kepler’s SNR favors a hadronic origin in GeV band. Through analyzing multi-band data from radio to γ-ray and surveying the distribution from the surrounding CO molecules cloud, we found that if this γ-ray emission is from Kepler’s SNR, then it may originate from interactions between the relativistic protons escaping from the shock of Kepler’s SNR and surrounding CO gas molecules. However, more observation data are necessary to firmly confirm the association between the γ-ray source and Kepler’s SNR in the future.
On the Use of Field RR Lyrae as Galactic Probes. II. A New ΔS Calibration to Estimate Their Metallicity*
Authors: Crestani J. , Fabrizio M. , Braga V. F. , Sneden C. , Preston G. , Ferraro I. , Iannicola G. , Bono G. , Alves-Brito A. , Nonino M. , D’Orazi V. , Inno L. , Monelli M. , Storm J. , Altavilla G. , Chaboyer B. , Dall’Ora M. , Fiorentino G. , Gilligan C. , Grebel E. K. , Lala H. , Lemasle B. , Marengo M. , Marinoni S. , Marrese P. M. , Martínez-Vázquez C. E. , Matsunaga N. , Mullen J. P. , Neeley J. , Prudil Z. , Silva R. da , Stetson P. B. , Thévenin F. , Valenti E. , Walker A. , Zoccali M. 
Published: February 2021

Abstract
We performed the largest and most homogeneous spectroscopic survey of field RR Lyraes (RRLs). We secured ≈6300 high-resolution (HR, R ∼ 35,000) spectra for 143 RRLs (111 fundamental, RRab; 32 first-overtone, RRc). The atmospheric parameters were estimated by using the traditional approach and the iron abundances were measured by using an LTE line analysis. The resulting iron distribution shows a well-defined metal-rich tail approaching solar iron abundance. This suggests that field RRLs experienced a complex chemical enrichment in the early halo formation. We used these data to develop a new calibration of the ΔS method. This diagnostic, based on the equivalent widths of Ca ii K and three Balmer (H
δ,γ,β
) lines, traces the metallicity of RRLs. For the first time, the new empirical calibration: (i) includes spectra collected over the entire pulsation cycle; (ii) includes RRc variables; (iii) relies on spectroscopic calibrators covering more than three dex in iron abundance; and (iv) provides independent calibrations based on one/two/three Balmer lines. The new calibrations were applied to a data set of both SEGUE-SDSS and degraded HR spectra totalling 6451 low-resolution (R ∼ 2000) spectra for 5001 RRLs (3439 RRab, 1562 RRc). This resulted in an iron distribution with a median η = −1.55 ± 0.01 and σ = 0.51 dex, in good agreement with literature values. We also found that RRc are 0.10 dex more metal-poor than RRab variables, and have a distribution with a smoother metal-poor tail. This finding supports theoretical prescriptions suggesting a steady decrease in the RRc number when moving from metal-poor to metal-rich stellar environments.
A Backscattering-dominated Prompt Emission Model for the Prompt Phase of Gamma-Ray Bursts
Authors: Vyas Mukesh K. , Pe’er Asaf , Eichler David 
Published: February 2021

Abstract
As a gamma-ray burst (GRB) jet drills its way through the collapsing star, it traps a baryonic “cork” ahead of it. Here we explore a prompt emission model for GRBs in which the jet does not cross the cork, but rather photons that are emitted deep in the flow largely by pair annihilation are scattered inside the expanding cork and escape largely from the back end of it as they push it from behind. Due to the relativistic motion of the cork, these photons are easily seen by an observer close to the jet axis peaking at ε
peak ∼ few ×100 keV. We show that this model naturally explains several key observational features: (1) a high-energy power-law index β
1 − 2 to − 5 with an intermediate thermal spectral region; (2) decay of the prompt emission light curve as ∼ t
−2; (3) delay of soft photons; (4) a peak energy–isotropic energy (the so-called “Amati”) correlation,

ε

peak

∼

ε

iso

m

, with m ∼ 0.45, resulting from different viewing angles (at low luminosities, our model predicts an observable turnoff in the Amati relation); (5) an anticorrelation between the spectral FWHM and time as t
−1; (6) temporal evolution ε
peak ∼ t
−1; and (7) distribution of peak energies ε
peak in the observed GRB population. The model is applicable for single-pulse GRB light curves and their respective spectra. We discuss the consequences of our model in view of current and future prompt emission observations.