bluuebunny/crossref_metadata_2025_split huggingface dataset:
Direct comparison of two extended half-life PEGylated recombinant FVIII products: a randomized, crossover pharmacokinetic study in patients with severe hemophilia A
Authors: Solms Alexander , Shah Anita , Berntorp Erik , Tiede Andreas , Iorio Alfonso , Linardi Camila , Ahsman Maurice , Mancuso Maria Elisa , Zhivkov Tihomir , Lissitchkov Toshko 
Published: September 2020

AbstractAn open-label, crossover randomized study was performed to compare the pharmacokinetics (PK) of damoctocog alfa pegol and rurioctocog alfa pegol, two recombinant factor VIII (FVIII) products indicated in patients with hemophilia A, both conjugated to polyethylene glycol to reduce clearance and extend time in circulation. Adult patients (N = 18) with severe hemophilia A (FVIII < 1 IU/dL), previously treated with any FVIII product for ≥ 150 exposure days, were randomized to receive a single 50 IU/kg infusion of damoctocog alfa pegol followed by rurioctocog alfa pegol, or vice versa, with ≥ 7-day washout between doses. FVIII activity was measured using the one-stage clotting assay. PK parameters, including area under the curve from time 0 to the last data point (AUC0–tlast, primary parameter), dose-normalized AUC (AUCnorm), and time to threshold, were calculated based on 11 time points between 0.25 and 120 h post-dose and evaluated using a noncompartmental model. Due to differences in batch-specific vial content used for the study, actual administered median doses were 54.3 IU/kg for damoctocog alfa pegol and 61.4 IU/kg for rurioctocog alfa pegol. Based on actual dosing, a significantly higher geometric mean (coefficient of variation [%CV]) AUCnorm was observed for damoctocog alfa pegol (43.8 h kg/dL [44.0]) versus rurioctocog alfa pegol (36.0 h kg/dL [40.1, P < 0.001]). Based on population PK modeling, median time to reach 1 IU/dL was 16 h longer for damoctocog alfa pegol compared with rurioctocog alfa pegol. No adverse events or any immunogenicity signals were observed. Overall, damoctocog alfa pegol had a superior PK profile versus rurioctocog alfa pegol. Trial registration number: NCT04015492 (ClinicalTrials.gov identifier). Date of registration: July 9, 2019
Recurrent laryngeal nerve monitoring during totally robot-assisted Ivor Lewis esophagectomy
Authors: Staubitz J. I. , van der Sluis P. C. , Berlth F. , Watzka F. , Dette F. , Läßig A. , Lang H. , Musholt T. J. , Grimminger P. P. 
Published: September 2020

Abstract
Purpose
The robot-assisted approach for Ivor Lewis esophagectomy offers an enlarged, three-dimensional overview of the intraoperative situs. The vagal nerve (VN) can easily be detected, preserved, and intentionally resected below the separation point of the recurrent laryngeal nerve (RLN). However, postoperative vocal cord paresis can result from vagal or RLN injury during radical lymph node dissection, presenting a challenge to the operating surgeon.

Methods
From May to August 2019, 10 cases of robot-assisted minimally invasive esophagectomy (RAMIE) with extended 2-field lymphadenectomy, performed at the University Medical Center Mainz, were included in a prospective cohort study. Bilateral intermittent intraoperative nerve monitoring (IONM) of the RLN and VN was performed, including pre- and postoperative laryngoscopy assessment.

Results
Reliable mean signals of the right VN (2.57 mV/4.50 ms) and the RLN (left 1.24 mV/3.71 ms, right 0.85 mV/3.56 ms) were obtained. IONM facilitated the identification of the exact height of separation of the right RLN from the VN. There were no cases of permanent postoperative vocal paresis. Median lymph node count from the paratracheal stations was 5 lymph nodes.

Conclusion
IONM was feasible during RAMIE. The intraoperative identification of the RLN location contributed to the accuracy of lymph node dissection of the paratracheal lymph node stations. RLN damage and subsequent postoperative vocal cord paresis can potentially be prevented by IONM.
Bank-Laine Functions with Real Zeros
Authors: Langley J. K. 
Published: September 2020

AbstractSuppose that E is a real entire function of finite order with zeros which are all real but neither bounded above nor bounded below, such that $$E'(z) = \pm 1$$

E
′

(
z
)

=
±
1

whenever $$E(z) = 0$$

E
(
z
)
=
0

. Then either E has an explicit representation in terms of trigonometric functions or the zeros of E have exponent of convergence at least 3. An example constructed via quasiconformal surgery demonstrates the sharpness of this result.
Development of an Ethnic Identity Measure for Americans of Middle Eastern and North African Descent: Initial Psychometric Properties, Sociodemographic, and Health Correlates
Authors: Resnicow Ken , Patel Minal R. , Green Molly , Smith Alyssa , Bacon Elizabeth , Goodell Stefanie , Tariq Madiha , Alhawli Asraa , Syed Nadia , Van Horn M. Lee , Stiffler Matthew 
Published: September 2020

Abstract
Background
Southeast Michigan is home to the second largest Middle Eastern and North African (MENA) US population. There is increasing interest in understanding correlates of psychosocial outcomes and health behaviors in this growing population. One potentially important health correlate is ethnic identity (EI). This paper reports the development, validity, and initial correlates of a new measure of MENA identity named the MENA-IM.

Methods
We used convenience sampling at locations frequented by individuals of MENA descent in southeast Michigan. We also measured EI centrality, religiosity, cultural mistrust, substance use, and health status to assess convergent and divergent validity. Exloratory and Confirmatory Factor Analysis identified three subscales, which were valid for both Arab and Chaldean respondents and were named (1) MENA cultural affiliation, (2) MENA media use, and (3) multicultural affiliation. We also created and tested a 20-item, single-factor version.

Results
We obtained data from 378 adults, 73% of whom identified as Arab and 27% as Chaldean. MENA-IM scores were higher among older, lower-educated, lower-income, non-US born, and Arabic-speaking respondents. Arab respondents reported significantly higher scores than Chaldeans. MENA-IM scores were positively associated with EI centrality and religiosity. Higher MENA-IM scores were found among those not reporting use of marijuana, alcohol, and opiates. Higher MENA-IM scores were also found among those without a self-reported history of heart disease and among those with better mental health status.

Discussion
The MENA-IM has strong psychometric properties and demonstrated initial evidence of convergent and discriminant validity. In general, values on the measure were associated with better psychosocial and health status. How the measure performs with MENA populations outside of Michigan and how it may relate to other health outcomes merit investigation.
Regulierung des Pflegemarktes: Räumliche Fehlentwicklungen werden verstärkt
Authors: Just Tobias , Plößl Franziska 
Published: September 2020

ZusammenfassungAngesichts der Alterung der deutschen Gesellschaft wird der Bedarf an Pflegedienstleistungen künftig zunehmen, und dies erzwingt, adäquate und bezahlbare Pflegekonzepte dort zu ermöglichen, wo der Bedarf entsteht. Drei idealtypische Pflegeheiminvestitionsbeispiele illustrieren, dass positive Projektgewinne in (sehr) zentralen Lagen schwerer zu erzielen sind als in der Peripherie. Dabei werden die Auswirkungen kritischer oder gesetzlich reglementierter Parameter, wie die maximale Heimgröße, auf die Rentabilität von Neubauvorhaben untersucht. Um diesen asymmetrisch wirkenden Anreizstrukturen entgegen zu wirken, könnte zum einen die Zugänglichkeit von Grundstücken in Ballungsräumen, z. B. durch städtebauliche oder erbbaurechtliche Verträge, erleichtert werden. Zum anderen könnten neben einheitlichen Mindeststandards die länderspezifischen Regelungen durch regionale Anpassungsfaktoren, zur Berücksichtigung der unterschiedlichen Preisniveaus für Bauland, flexibler ausgestaltet werden.
Theory of Allosteric Regulation in Hsp70 Molecular Chaperones
Authors: Hendrickson Wayne A. 
Published: September 2020

AbstractHeat-shock proteins of 70 kDa (Hsp70s) are ubiquitous molecular chaperones that function in protein folding as well as other vital cellular processes. They bind and hydrolyze ATP in a nucleotide-binding domain (NBD) to control the binding and release of client polypeptides in a substrate-binding domain (SBD). However, the molecular mechanism for this allosteric action has remained unclear. Here, we develop and experimentally quantify a theoretical model for Hsp70 allostery based on equilibria among Hsp70 conformational states. We postulate that, when bound to ATP, Hsp70 is in equilibrium between a restraining state (R) that restricts ATP hydrolysis and binds peptides poorly, if at all, and a stimulating state (S) that hydrolyzes ATP relatively rapidly and has high intrinsic substrate affinity but rapid binding kinetics; after the hydrolysis to ADP, NBD and SBD disengage into an uncoupled state (U) that binds peptide substrates tightly, but now with slow kinetics of exchange.
When Social Capital Becomes Political Capital: Understanding the Social Contexts of Minority Candidates' Electoral Success in the American States
Authors: Wright Kenicia , Zhu Ling 
Published: September 2020

AbstractPolitical scientists have long been interested in studying the elective office-holding of disadvantaged groups. However, this line of research primarily focuses on the representation of ethnic minorities in the U.S. Congress and identifies three types of determinants of minority candidates' electoral success: the demographic and political make-up of constituents, candidates' personal traits, and macro-level electoral rules. Much less attention is given to minority candidates' electoral success in statehouses. In this paper, we ask: what factors promote the electoral success of minority candidates in state legislatures? Beyond voter characteristics and electoral rules, we attribute minority candidates' electoral success to the social capital possessed by their in-group constituents. We theorize that social capital manifested as civic engagement and social connectedness, can become political capital for minority candidates. Using the Current Population Surveys Civic Engagement Supplement, we validate state-level measures of social capital by race and ethnicity. Linking group social capital to state legislative election outcomes, we find the stock of minority social capital contributes to the electoral success of minority candidates, while white social capital decreases minority candidates' electoral success. Key findings suggest social capital is a form of political capital for disadvantaged groups with private benefits for in-group candidates.
Impact of small-scale emerging flux from the photosphere to the corona: a case study from IRIS
Authors: Guglielmino Salvo L. , Young Peter R. , Zuccarello Francesca , Romano Paolo , Murabito Mariarita 
Published: September 2020

AbstractWe report on multi-wavelength ultraviolet (UV) high-resolution observations taken with the IRIS satellite during the emergence phase of an emerging flux region embedded in the unipolar plage of active region NOAA 12529. These data are complemented by measurements taken with the spectropolarimeter aboard the Hinode satellite and by observations from SDO.In the photosphere, we observe the appearance of opposite emerging polarities, separating from each other, and cancellation with a pre-existing flux concentration of the plage.In the upper atmospheric layers, recurrent brightenings resembling UV bursts, with counterparts in all UV/EUV filtergrams, are identified in the EFR site. In addition, plasma ejections are observed at chromospheric level. Most important, we unravel a signature of plasma heated up to 1 MK detecting Fe XII emission in the core of the brightening sites.Comparing these findings with previous observations and numerical models, we suggest evidence of several long-lasting, small-scale magnetic reconnection episodes between the new bipolar EFR and the ambient field.
Could star-planet magnetic interactions lead to planet migration and influence stellar rotation?
Authors: Ahuir Jérémy , Strugarek Antoine , Brun Allan Sacha , Mathis Stéphane , Bolmont Emeline , Benbakoura Mansour , Réville Victor , Le Poncin-Lafitte Christophe 
Published: September 2020

AbstractThe distribution of hot Jupiters, for which star-planet interactions can be significant, questions the evolution of exosystems. We aim to follow the orbital evolution of a planet along the rotational and structural evolution of the host star by taking into account the coupled effects of tidal and magnetic torques from ab initio prescriptions. It allows us to better understand the evolution of star-planet systems and to explain some properties of the distribution of observed close-in planets. To this end we use a numerical model of a coplanar circular star-planet system taking into account stellar structural changes, wind braking and star-planet interactions, called ESPEM (Benbakoura et al. (2019)). We find that depending on the initial configuration of the system, magnetic effects can dominate tidal effects during the various phases of the evolution, leading to an important migration of the planet and to significant changes on the rotational evolution of the star. Both kinds of interactions thus have to be taken into account to predict the evolution of compact star-planet systems.
Cycle times of early M dwarf stars: mean field models versus observations
Authors: Küker Manfred , Rüdiger Günther , Oláh Katalin , Strassmeier Klaus G. 
Published: September 2020

AbstractObservations of early-type M stars suggest that there are two characteristic cycle times, one of order one year for fast rotators (Prot < 1 day) and another of order four years for slower rotators. For a sample of fast-rotating stars, the equator-to-pole differences of the rotation rates up to 0.03 rad d−1 are also known from Kepler data. These findings are well-reproduced by mean field models. These models predict amplitudes of the meridional flow, from which the travel time from pole to equator at the base of the convection zone of early-type M stars can be calculated. As these travel times always exceed the observed cycle times, our findings do not support the flux transport dynamo.
Coordinated observations between China and Europe to follow active region 12709
Authors: Manrique S. J. González , Kuckein C. , Gömöry P. , Yuan S. , Xu Z. , Rybák J. , Balthasar H. , Schwartz P. 
Published: September 2020

AbstractWe present the first images of a coordinated campaign to follow active region NOAA 12709 on 2018 May 13 as part of a joint effort between three observatories (China-Europe). The active region was close to disk center and enclosed a small pore, a tight polarity inversion line and a filament in the chromosphere. The active region was observed with the 1.5-meter GREGOR solar telescope on Tenerife (Spain) with spectropolarimetry using GRIS in the He i 10830 Å spectral range and with HiFI using two broad-band filter channels. In addition, the Lomnicky Stit Observatory (LSO, Slovakia) recorded the same active region with the new Solar Chromospheric Detector (SCD) in spectroscopic mode at Hα 6562 Å. The third ground-based telescope was located at the Fuxian Solar Observatory (China), where the active region was observed with the 1-meter New Vacuum Solar Telescope (NVST), using the Multi-Channel High Resolution Imaging System at Hα 6562 Å. Overlapping images of the active region from all three telescopes will be shown as well as preliminary Doppler line-of-sight (LOS) velocities. The potential of such observations are discussed.
On the Role of Magnetic Fields in an Erupting Solar Filament
Authors: Song Qiao , Yang Shuhong , Wang Jing-Song 
Published: September 2020

AbstractA filament eruption may lead to a coronal mass ejection (CME), which is one of the main driving mechanisms of space weather. This work analyses a slow and flareless CME event associated with an erupting quiescent filament. By using the extreme ultraviolet images of the Atmospheric Imaging Assembly onboard the Solar Dynamics Observatory, we trace the evolution of the filament in detail, and present the manifestations of the role of magnetic fields in the low corona. The results suggest the existence of a magnetic flux rope in the pre-eruption structures. Our study of this complex magnetic system may lead to a better understanding of CMEs and their impact on the space weather.
Characterization of stellar activity using transits and its impact on habitability
Authors: Estrela Raissa , Valio Adriana , Palit Sourav 
Published: September 2020

AbstractStellar magnetic field is the driver of activity in stars and can trigger spots, energetic flares, coronal plasma ejections and ionized winds. These phenomena play a crucial role in understanding the internal mechanisms of the star, but can also have potential effects in orbiting planets. During the transit of a planet, spots can be occulted producing features imprinted in the transit light curve. Here, we modelled these features to characterize the physical properties of the spots (radius, intensity, and location). In addition, we monitor spots signatures on multiple transits to estimate magnetic cycles length of Kepler stars. Flares have also been observed during transits in active stars. We derive the properties of the flares and analyse their UV impact on possible living organisms in planets orbiting in the habitable zone.
New Candidates for Chromospherically Young, Kinematically Old Stars
Authors: Machado Pereira Eduardo , Rocha Pinto Helio J. 
Published: September 2020

AbstractRoughly speaking, young stars are associated to intense chromospheric activity (CA), whereas it decreases with stellar aging. However, some objects that show high kinematical components – in turn, associated to older stars – reveal CA similar to that of young ones; we call these stars chromospherically young and kinematically old (CYKOs). One hypothesis that could explain their occurrence is the merge of a short-period binary, from which the outcome would be a chromospherically active, kinematically evolved star. Considering that they evolved separately, we expect them to be lithium depleted, and therefore we look for CYKO stars by analyzing their lithium content (λ 6707 Å). We present a preliminary list of 48 stars matching this criteria, aiming to either confirm or discard the coalescence of a short-period pair hypothesis.
Examining the optical intensity and magnetic field expansion factor in the open magnetic field regions associated with coronal holes
Authors: Lin Chia-Hsien , Huang Guan-Han , Lee Lou-Chuang 
Published: September 2020

AbstractCoronal holes can be identified as the darkest regions in EUV or soft X-ray images with predominantly unipolar magnetic fields (LIRs) or as the regions with open magnetic fields (OMF). Our study reveals that only 12% of OMF regions are coincident with LIRs. The aim of this study is to investigate the conditions that affect the EUV intensity of OMF regions. Our results indicate that the EUV intensity and the magnetic field expansion factor of the OMF regions are weakly positively correlated when plotted in logarithmic scale, and that the bright OMF regions are likely to locate inside or next to the regions with closed field lines. We empirically determined a linear relationship between the expansion factor and the EUV intensity. The relationship is demonstrated to improve the consistency from 12% to 23%. The results have been published in Astrophysical Journal (Huang et al. 2019).
Semi-empirical 2D model of the solar corona and solar wind using solar eclipse images: Progress report
Authors: Sittler Edward C. , Sittler Linda M. 
Published: September 2020

AbstractWe present white light images of the Sun's corona acquired during the total Solar Eclipses on August 21, 2017 in mountains north of Boise Idaho USA and on July 2, 2019 south of Copiapo Chile. In both cases the viewing was excellent, altitudes ∼ 1200 m and relative humidity ∼ 10. We used an Orion equatorial reflecting telescope with 203 mm diameter aperture and 1000 mm focal length for f4.9 optics. A computer-controlled Canon EOS Rebel T3i digital camera was used. We plan to use our 2019 eclipse images for analysis since the Sun is near solar minimum so 2D steady state MHD equations can be used. We present a plan to process the images and convert them into a 2D empirical model of electron density and magnetic field in radial distance and co-latitude, from which 2D maps of flow velocity, effective temperature and effective heat flux can be computed.
Global simulations of stellar dynamos
Authors: Guerrero G. 
Published: September 2020

AbstractThe dynamo mechanism, responsible for the solar magnetic activity, is still an open problem in astrophysics. Different theories proposed to explain such phenomena have failed in reproducing the observational properties of the solar magnetism. Thus, ab-initio computational modeling of the convective dynamo in a spherical shell turns out as the best alternative to tackle this problem. In this work we review the efforts performed in global simulations over the past decades. Regarding the development and sustain of mean-flows, as well as mean magnetic field, we discuss the points of agreement and divergence between the different modeling strategies. Special attention is given to the implicit large-eddy simulations performed with the EULAG-MHD code.
Magnetic field evolution in solar-type stars
Authors: Brandenburg Axel 
Published: September 2020

AbstractWe discuss selected aspects regarding the magnetic field evolution of solar-type stars. Most of the stars with activity cycles are in the range where the normalized chromospheric Calcium emission increases linearly with the inverse Rossby number. For Rossby numbers below about a quarter of the solar value, the activity saturates and no cycles have been found. For Rossby numbers above the solar value, again no activity cycles have been found, but now the activity goes up again for a major fraction of the stars. Rapidly rotating stars show nonaxisymmetric large-scale magnetic fields, but there is disagreement between models and observations regarding the actual value of the Rossby number where this happens. We also discuss the prospects of detecting the sign of magnetic helicity using various linear polarization techniques both at the stellar surface using the parity-odd contribution to linear polarization and above the surface using Faraday rotation.
Resolving Power of Asteroseismic Inversion of the Kepler Legacy Sample
Authors: Kosovichev Alexander G. , Kitiashvili Irina N. 
Published: September 2020

AbstractThe Kepler Asteroseismic Legacy Project provided frequencies, separation ratios, error estimates, and covariance matrices for 66 Kepler main sequence targets. Most of the previous analysis of these data was focused on fitting standard stellar models. We present results of direct asteroseismic inversions using the method of optimally localized averages (OLA), which effectively eliminates the surface effects and attempts to resolve the stellar core structure. The inversions are presented for various structure properties, including the density stratification and sound speed. The results show that the mixed modes observed in post-main sequence F-type stars allow us to resolve the stellar core structure and reveal significant deviations from the evolutionary models obtained by the grid-fitting procedure to match the observed oscillation frequencies.