bluuebunny/crossref_metadata_2025_split huggingface dataset:
Panamá
Authors: Fisher Eloy 
Published: March 2020

Este documento de posición analiza el crecimiento y la inflación en Panamá. Panamá experimenta un círculo virtuoso económico entre una tasa balanceada y sostenible de crecimiento a largo plazo y ni-veles moderados de inflación, fenómeno que los economistas denominan la coincidencia divina. A futuro, con el repliegue gradual del rol del Estado en aras de fortalecer la actividad del sector privado, se dan las condiciones macroeconómicas para mantener y recrear tal coincidencia como la nueva si-tuación normal de la economía panameña. La diversificación de la economía, la prudencia macro-fiscal, perspectivas favorables de crecimiento en sectores claves (como lo son las utilidades públicas, minas y canteras, y transporte, almacenamiento y comunicaciones —sectores a su vez dependientes del comercio internacional y la exportación de servicios) y la reversión a la media de la inflación, incluso a pesar de la incertidumbre económica internacional y geopolítica, constituyen pilares sólidos sobre los cuales descansa la actividad económica y el modelo de desarrollo del país. Se concluye con advertencias sobre el posible agotamiento del modelo de gasto discrecional en materia social, ya que los réditos de estas intervenciones han perdido potencia y en la medida que no se re-enfoquen, podrían trastocar el delicado equilibrio necesario para mantener y enraizar la coincidencia divina a nivel eco-nómico. Por eso, se concluye que la mejor política hoy en día debe ser prudente y cautelosa, y enfocada a generar capital social.
This position paper analyzes the growth and inflation in Panama. Panama experiences a virtuous circle for economy: a balanced and sustained rate of long-term growth, and moderate levels of inflation. This phenomenon is what economists call the divine coincidence. As the role of the Government withdraws gradually, in order to strengthen the activity of the private sector, the macroeconomic conditions to sustain and recreate such coincidence as the new normal situation of the Panamanian economy will emerge. The diversification of the economy, the macro-fiscal prudence, the favorable perspectives of growth in key sectors (such as public utilities, mines and quarries, and transport, storage and communications; which are sectors that depend upon international commerce and service exports), and the mean reversion of inflation —even despite the economic and geopolitical uncertainties— are the cornerstones upon which the economic activity and the development model of the nation lay. Warnings about the possible wears of the model of discretionary expenditure in social fields, since the revenues of these interventions have lost power. If there is no shift in the focus of these interventions, they could disrupt the delicate balance needed to maintain and strengthen the divine coincidence at the economic level. Thus, the best policy today must be prudent, cautious and focused to develop social capital.
La nueva agenda de derechos humanos para la igualdad y el desarrollo humano sostenible.
Authors: Herrera Luis Carlos 
Published: March 2020

En los derechos humanos de primera generación; el interés era incorporar las libertades fundamenta-les, los derechos civiles, patrimoniales y políticos del individuo, para poner límites al poder del Estado. Los derechos de segunda generación son de contenido social para procurar las mejores condiciones de vida a las personas. Los derechos de tercera generación son derechos colectivos o derechos de los pueblos. Una nueva agenda de derechos humanos es la única forma de alcanzar un desarrollo soste-nible, donde el ser humano sea el centro del actuar nacional, regional y global. Debe ser holística, articuladora, universal, indivisible, multicultural, pluriétnica, con enfoque de género, inclusiva, con participación ciudadana, seguridad jurídica, solidaridad y cooperación internacional; que incluya estra-tegias y políticas públicas de respeto y garantía de los derechos de todas las personas, con especial protección a los grupos vulnerables. La eliminación de la violación a los derechos humanos —discri-minación de género, violencia contra la mujer, inseguridad, hambre, pobreza, el deterioro al medio ambiente, desigualdad social, la falta de acceso a la justicia, la migraciones, los efectos del cambio climático, la seguridad alimentaria, la educación de excelencia, la salud integral, el agua, la vivienda— son prioridades en una nueva agenda.
A COMPARISON BETWEEN TRANSURETHRAL CYSTOLITHOCLASTY AND VESICOLITHOTOMY IN PEDIATRIC MALE PATIENTS
Authors: Muhammed khalid  , Muhammad Faizan  , Muhammad Asif Gurmani  , Amjad Ali Siddiqui  , Qadeer Ahmed Choudhary  , Zulﬁqar Anjum  
Published: March 2020

ABSTRACT
BACKGROUND & OBJECTIVE: To compare transurethral cystolithoclasty with ureteroscope over open vesicolithotomy in pediatric male patients.
METHODOLOGY: Study comprises of hundred pediatric male patients, divided into two equal groups of 50 each, labeled as Group-A and Group-B. All the patients having stones less than 20mm size (average 14mm) were included. Group-A patients were treated with transurethral cystolithoclasty by using ureteroscope and pneumatic lithoclast assisted with the help of Dormia basket. Group-B patients were treated with open vesicolithotomy.RESULTS: All hundred male pediatric patients were between the ages of 1-15 years (mean age 8 years). Hospital stay was 2-3 days (average 2.5 days) in Group-A patients and 3-5 days (average 4 days) in Group-B patients. In Group-A3 (6%) patients had urinary tract infection, 1(2%) had urethral injury and 2(4%) had residual stone post-operatively. While Group-B4 (8%) suﬀered from urinary tract infection, 1(2%) had wound infection, 1(2%) had hematuria, and 2(4%) had fever. Retention of urine was 1(2%) in each Group.
CONCLUSION: Transurethral cystolithoclasty is a much better way of treating vesical calculus in pediatric male patients because it is a procedure with short hospital stay, minimal invasion, no scar and less complication. KEYWORDS: Bladder Calculus, Comparison, Cystolithoclasty, Ureteroscope, Pneumatic Lithoclast, Dormia basket, Vesicolithotomy.
KARAKTERISTIK IBU BERSALIN DENGAN INDIKASI SECTIO CAESAREA TAHUN 2012-2013 DI MEDICAL RECORD RSUD ARIFIN ACHMAD PEKANBARU
Authors: Maswarni Maswarni , Kumalasari Ayu 
Published: March 2020

Sectio caesarea adalah pembedahan untuk melahirkan janin dengan membuka dinding perut dan dinding rahim. Tujuan penelitian: untuk mengetahui karakteristik ibu bersalin dengan indikasi sectio caesarea Tahun 2012-2013 di medical record RSUD Arifin Achmad Pekanbaru. Metodologi penelitian: jenis penelitian deskriptif, digunakan data sekunder yaitu seluruh ibu bersalin dengan indikasi sectio caesarea yang terdata di medical record RSUD Arifin Achmad Pekanbaru yang dilakukan pada tanggal 01-15 September 2014. Populasi dan sampel: seluruh data ibu bersalin dengan indikasi sectio caesarea sebanyak 319 ibu bersalin, dengan menggunakan lembar checklist. Analisis data: analisa Univariete. Hasil penelitian: karakteristik ibu bersalin dengan indikasi sectio caesarea tahun 2012-2013 adalah berdasarkan umur, pendidikan, pekerjaan, paritas, dan indikasi. Dimana umur adalah mayoritas umur 20-35 tahun sebanyak 243 responden (76,18%), dari pendidikan mayoritas SMA sebanyak 157 responden (49,22%), dari pekerjaan mayoritas IRT (Ibu Rumah Tangga) sebanyak 296 responden (92,79%), sedangkan dari paritas mayoritas multipara sebanyak 184 responden (57,68%), dan dari indikasi mayoritas Chepalo Pelvik Disproportion (CPD) sebanyak 65 responden (20,38%). Diharapkan kepada para petugas kesehatan RSUD Arifin Achmad Pekanbaru agar pelayanan dan evaluasi tindakan sectio caesarea meningkat, sehingga kejadian sectio caesarea dapat ditekan.
Quantitative and Qualitative Results from Orbital Plane Precession of Medium-high Near-circular Orbits
Authors: Zhang Ming-Jiang , Zhao Chang-Yin , Xiong Jian-Ning , Zhu Ting-Lei , Zhang Wei 
Published: March 2020

Abstract
The theoretical analysis of Allan & Cook on the mechanisms of orbital plane precession for medium-high circular orbits is briefly reviewed, and the fact that there are two types of possible precession mechanisms (not only the classical Laplace precession) for the long-term evolution of the orbital plane of medium-high near-circular orbits is especially emphasized. Based on two types of possible precession mechanisms, the analytical formulae of the quantitative variation ranges of orbital inclination derived by Zhao et al. are revised, and the complete analytical formulae for medium-high near-circular orbits are obtained. The qualitative characteristic formula for the variation of orbital inclination-longitude of the ascending node of geostationary orbits in Zhao et al. is generalized to medium-high near-circular orbits, and the more general analytical formulae are obtained. Taking the near-circular orbits with the altitudes as the geosynchronous and medium orbits of the BeiDou navigation satellites as examples, the theoretically quantitative and qualitative results from orbital plane precession are verified by the first-order semianalytical calculations with simplified models and numerical calculations with precise models to a certain extent. Moreover, the specific quantitative and qualitative results for medium-high near-circular orbits with the given initial inclinations and different initial longitudes of the ascending node are particularly presented, from which some conclusions are summarized. Due to the high similarity of orbital plane precession for natural satellites to that of artificial satellites, the results and methodology in this paper can be directly extended to the long-term evolution of the orbital plane for natural satellites and help to understand and explain some orbit dynamic phenomena of natural satellites.
Explosions Driven by the Coalescence of a Compact Object with the Core of a Massive-star Companion inside a Common Envelope: Circumstellar Properties, Light Curves, and Population Statistics
Authors: Schrøder Sophie Lund , MacLeod Morgan , Loeb Abraham , Vigna-Gómez Alejandro , Mandel Ilya 
Published: March 2020

Abstract
We model explosions driven by the coalescence of a black hole or neutron star with the core of its massive-star companion. Upon entering a common-envelope phase, a compact object may spiral all the way to the core. The concurrent release of energy is likely to be deposited into the surrounding common envelope, powering a merger-driven explosion. We use hydrodynamic models of binary coalescence to model the common-envelope density distribution at the time of coalescence. We find toroidal profiles of material, concentrated in the binary’s equatorial plane and extending to many times the massive star’s original radius. We use the spherically averaged properties of this circumstellar material (CSM) to estimate the emergent light curves that result from the interaction between the blast wave and the CSM. We find that typical merger-driven explosions are brightened by up to three magnitudes by CSM interaction. From population synthesis models, we discover that the brightest merger-driven explosions, M

V
∼ −18 to −20, are those involving black holes because they have the most massive and extended CSM. Black hole coalescence events are also common; they represent about 50% of all merger-driven explosions and approximately 0.25% of the core-collapse rate. Merger-driven explosions offer a window into the highly uncertain physics of common-envelope interactions in binary systems by probing the properties of systems that merge rather than eject their envelopes.
Energetic Ion Dynamics Near the Cusp Region of Mercury
Authors: Jang E. , Zhao J.–T. , Yue C. , Zong Q.–G. , Liu Y. , Liu Z.–Y. 
Published: March 2020

Abstract
Energetic ions in Mercury’s magnetosphere are very dynamic, similar to those in the magnetosphere of Earth. In this study, we present two energetic proton observations by MErcury Surface, Space ENvironment, GEochemistry and Ranging near the cusp region of Mercury. For one case, we have observed a large flux of energetic protons while the other case has almost no flux, indicating that the near-cusp region may trap energetic particles under particular conditions. In order to understand under what conditions the near-cusp region of Mercury could trap energetic particles, we have used test particle simulations to trace the trajectories of single particles of different energies and pitch angles with a magnetic field model, KT17, that could closely represent the observed in situ magnetic field. Under different magnetic field geometries, the motions of single particles with various energies and pitch angles are different. The test particles can be trapped around the cusp region when the solar disturbance activity that generates the magnetic field local minimum near the cusp region is strong, while the particles cannot be trapped and escape along the magnetic field through the dawnside cusp when there is little solar activity.
Spectroscopic Confirmation of a Coma Cluster Progenitor at z ∼ 2.2
Authors: Darvish Behnam , Scoville Nick Z. , Martin Christopher , Sobral David , Mobasher Bahram , Rettura Alessandro , Matthee Jorryt , Capak Peter , Chartab Nima , Hemmati Shoubaneh , Masters Daniel , Nayyeri Hooshang , O’Sullivan Donal , Paulino-Afonso Ana , Sattari Zahra , Shahidi Abtin , Salvato Mara , Lemaux Brian C. , Fèvre Olivier Le , Cucciati Olga 
Published: March 2020

Abstract
We report the spectroscopic confirmation of a new protocluster in the COSMOS field at z ∼ 2.2, COSMOS Cluster 2.2 (CC2.2), originally identified as an overdensity of narrowband selected Hα emitting candidates. With only two masks of Keck/MOSFIRE near-IR spectroscopy in both H (∼1.47–1.81 μm) and K (∼1.92–2.40 μm) bands (∼1.5 hr each), we confirm 35 unique protocluster members with at least two emission lines detected with S/N > 3. Combined with 12 extra members from the zCOSMOS-deep spectroscopic survey (47 in total), we estimate a mean redshift and a line-of-sight velocity dispersion of z
mean = 2.23224 ± 0.00101 and σ
los = 645 ± 69 km s−1 for this protocluster, respectively. Assuming virialization and spherical symmetry for the system, we estimate a total mass of M
vir ∼ (1–2) ×1014
M
⊙ for the structure. We evaluate a number density enhancement of δ

g
∼ 7 for this system and we argue that the structure is likely not fully virialized at z ∼ 2.2. However, in a spherical collapse model, δ

g
is expected to grow to a linear matter enhancement of ∼1.9 by z = 0, exceeding the collapse threshold of 1.69, and leading to a fully collapsed and virialized Coma-type structure with a total mass of M
dyn(z = 0) ∼ 9.2 × 1014
M
⊙ by now. This observationally efficient confirmation suggests that large narrowband emission-line galaxy surveys, when combined with ancillary photometric data, can be used to effectively trace the large-scale structure and protoclusters at a time when they are mostly dominated by star-forming galaxies.
On the (Lack of) Evolution of the Stellar Mass Function of Massive Galaxies from z = 1.5 to 0.4
Authors: Kawinwanichakij Lalitwadee , Papovich Casey , Ciardullo Robin , Finkelstein Steven L. , Stevans Matthew L. , Wold Isak G. B. , Jogee Shardha , Sherman Sydney , Florez Jonathan , Gronwall Caryl 
Published: March 2020

Abstract
We study the evolution in the number density of galaxies at the highest stellar masses over the past ≈9 Gyr (

) using the Spitzer/HETDEX Exploratory Large-Area Survey (SHELA). SHELA includes complete imaging in eight photometric bands spanning 0.3–4.5 μm over 17.5 deg2 within the SDSS Stripe 82 field. The size of SHELA produces the lowest counting uncertainties and cosmic variance yet for massive galaxies at z ∼ 1.0. We study the evolution in the intrinsic stellar mass function (SMF) for galaxies with

using a forward-modeling method that takes into full account the statistical and systematic uncertainties on stellar mass. From z = 0.4 to 1.5, the evolution in the massive end of the intrinsic SMF shows minimal change in its shape: the characteristic mass (M*) evolves by less than 0.1 dex (±0.05 dex); furthermore, the number density of galaxies with

11 stays roughly constant at

(±0.05) from z = 1 to z = 0.4, consistent with no evolution, then declines to

= −3.7 (±0.05) at z = 1.5. We discuss the uncertainties in the derived SMF, which are dominated by assumptions in the star formation history and details of stellar population synthesis models for stellar mass estimations. We also study the evolution in the SMF for samples of star-forming and quiescent galaxies selected by their specific star formation rate. For quiescent galaxies, the data are consistent with no (or slight) evolution (≲0.1 dex) in either the characteristic mass or number density from z ∼ 1.5 to the present even after accounting for the systematic uncertainty and the random error in the stellar mass measurement. The lack of number density evolution in the quiescent massive galaxy population means that any mass growth (presumably through “dry” mergers) must balance the rate of stellar mass losses owing to processes of late-stage stellar evolution and the formation of newly quiescent galaxies from the star-forming population. We provide an upper limit on this mass growth from z = 1.0 to 0.4 of ΔM
*/M
* = 45% (i.e., ≃0.16 dex) for quiescent galaxies more massive than 1011
M
⊙.
Effects of Orbital Eccentricity and IMF Cone Angle on the Dimensions of Mercury’s Magnetosphere
Authors: Zhong J. , Shue J.-H. , Wei Y. , Slavin J. A. , Zhang H. , Rong Z. J. , Chai L. H. , Wan W. X. 
Published: March 2020

Abstract
We investigate the influence of orbital eccentricity and interplanetary magnetic field (IMF) direction on the dimensions of Mercury’s magnetosphere using four Earth years of data collected by the MErcury Surface, Space ENvironment, GEochemistry, and Ranging spacecraft. The variations in magnetopause subsolar distance, flank distance, and tail radius are compared to determine the global dimensions and compressibility of the magnetosphere. As Mercury moves from perihelion (aphelion) to aphelion (perihelion) its magnetosphere expands (contracts) globally by ∼15% on average. After mapping all of the magnetopause crossings to a fixed radial distance from the Sun, we find that IMF cone angle changes lead to reconfigurations of the magnetosphere of comparable magnitude to radial solar distance effects. Furthermore, the magnetosphere is found to expand globally under the quasi-radial IMF, while contracting under the quasi-perpendicular conditions. A new Mercury magnetopause model parameterized by the heliocentric distance and IMF cone angle was constructed. Unlike Earth, the model gives a closed magnetopause for the nightside in most cases, and its flaring decreases with the contraction of the magnetosphere. The results demonstrate the highly variable reconfigurations of Mercury’s magnetosphere under its extreme environmental conditions.
The Regulation of Galaxy Growth along the Size–Mass Relation by Star Formation, as Traced by Hα in KMOS3D Galaxies at 0.7 ≲ z ≲ 2.7*
Authors: Wilman David J. , Fossati Matteo , Mendel J. Trevor , Saglia Roberto , Wisnioski Emily , Wuyts Stijn , Schreiber Natascha Förster , Beifiori Alessandra , Bender Ralf , Belli Sirio , Übler Hannah , Lang Philipp , Chan Jeffrey C. C. , Davies Rebecca L. , Nelson Erica J. , Genzel Reinhard , Tacconi Linda J. , Galametz Audrey , Davies Richard I. , Lutz Dieter , Price Sedona , Burkert Andreas , Tadaki Ken-ichi , Herrera-Camus Rodrigo , Brammer Gabriel , Momcheva Ivelina , Dokkum Pieter van 
Published: March 2020

Abstract
We present half-light sizes measured from

emission tracing star formation in 281 star-forming galaxies from the

survey at

. Sizes are derived by fitting 2D exponential disk models, with bootstrap errors averaging 20%.

sizes are a median (mean) of 1.19 (1.26) times larger than those of the stellar continuum—which, due to radial dust gradients, places an upper limit on the growth in stellar size via star formation—with just

intrinsic scatter. At fixed continuum size the

size shows no residual trend with stellar mass, star formation rate, redshift, or morphology. The only significant residual trend is with the excess obscuration of

by dust, at fixed continuum obscuration. The scatter in continuum size at fixed stellar mass is likely driven by the scatter in halo spin parameters. The stability of the ratio of

size to continuum size demonstrates a high degree of stability in halo spin and in the transfer of angular momentum to the disk over a wide range of physical conditions and cosmic time. This may require local regulation by feedback processes. The implication of our results, as we demonstrate using a toy model, is that our upper limit on star-formation-driven growth is sufficient only to evolve star-forming galaxies approximately along the observed size–mass relation, consistent with the size growth of galaxies at constant cumulative comoving number density. To explain the observed evolution of the size–mass relation of star-forming disk galaxies, other processes, such as the preferential quenching of compact galaxies or galaxy mergers, may be required.
Reducing the Data Rate in Internet of Things Applications by Using Wireless Sensor Network
Authors: Yahya Omar Hashim , Alrikabi Haider , Aljazaery Ibtisam A. 
Published: March 2020

Du to the raising number of using Internet of Things (I O T) for personal and commercial devices and applications, as well as the continues needs for improving the quality of the performance for the internet – connected devices enhance the researchers to investigate solutions for managing the data through the network Because of the fact that the internet-connected devices needs addresses for each sensor node uses the IP-network and a large number of electronic modules is fabricated to be compatible with IPv4 only like NodeMcu, ESP8266, Arduino WIFI, and ESP32 with knowing that the IPv4 has a limited addresses number that will not be enough for the needs of IOT developments, Many researchers turned to IPv6. In the proposed system, another solution is suggested instead of the IPV6. The proposed idea is based on Non-IP Wireless Sensor Network (WSN) by connecting many sensing nodes to the sink-node that has an IP to forward the data to the server to be visualized in a web-portal. By this method, it is able to connect more than one node to the internet over only one IP, there for the data rate that are needed will be decreased. In addition, by using the non-IP network, the data rate and the power consuming by the sensor nodes have been reduced, the practical results are discussed for connecting four nodes over one IP4 and how it will reduce the data rate and the power consuming. In this work, the esp33 has been used as a Sink-node, and the wireless transceiver module( NRF24) has been utilized to transmit the data from nodes to esp32.