bluuebunny/crossref_metadata_2025_split huggingface dataset:
Surgical intervention for late gastric conduit obstruction
Authors: Andrew Caroline D , Madariaga Maria Lucia L , Mathisen Douglas J , Morse Christopher R , Gaissert Henning A 
Published: June 2021

Abstract

OBJECTIVES
Gastric emptying delay after oesophagectomy may occur in conduits exposed to pleural forces of respiration or anatomic obstruction. Remedial operations addressing both causes are rarely reported. The study aim was to categorize severe gastric conduit obstruction (GCO) and report the outcome of surgical revision.

METHODS
A single-institution, retrospective study of gastric conduit revision following oesophagectomy for oesophageal cancer investigated incidence, risk factors and categories of conduit obstruction. Evaluation consisted of contrast studies, computed tomogram and endoscopy. Interventions were categorized according to obstructive cause and included pyloroplasty, hiatal hernia reduction and thoraco-abdominal conduit repositioning.

RESULTS
Among 1246 oesophagectomies over a 17-year period, 14 patients (1.1%) required post-oesophagectomy relief of GCO. Two additional patients presented after oesophagectomy elsewhere. Before oesophagectomy, 18.8% (3/16) and 62.5% (10/16) of patients were on chronic opioid and psychotropic medications, respectively. Distinct anatomic features separated obstruction into 3 categories: pyloric in 31% (5/16), extrinsic in 12.5% (2/16) and combined in 56.3% (9/16). Operative revision led to complete symptom resolution in 50% (8/16) of patients and symptom improvement in 43.8% (7/16) of patients. One patient (1/16, 6.25%) in the combined obstruction group did not improve with surgical revision.

CONCLUSIONS
GCO after oesophagectomy rarely requires surgical revision. Potential association with medications affecting oesophageal and gastric motility requires further investigation. Classification of obstruction identifies a patient subset with lower success after surgical revision.
Structure, composition and biological properties of fungal extracellular vesicles
Authors: Rizzo Juliana , Taheraly Adam , Janbon Guilhem 
Published: June 2021

ABSTRACTExtracellular vesicles (EVs) are lipidic nanosized particles that deliver a highly complex molecular cargo between cells and organisms and may serve numerous functions in intercellular communication, thereby influencing the evolution of microbial communities. Their roles in infectious diseases have been studied for a long time, comprising viral, bacterial, parasitic and to a less extent, fungal infections. Over the last few years, fungal EVs have become an increasingly active research field. Nevertheless, the understanding of EV functions during fungal infections poses challenging points, comprising the genetics regulating EV release, the EV structural and compositional complexity, the heterogeneity of the EV populations and their impact on host-pathogen interactions. This review explores the state-of-the-art investigations on fungal EVs and how this fast-evolving field can impact the development of new tools to fight fungal infections.
Loss of DRC1 function leads to multiple morphological abnormalities of the sperm flagella and male infertility in human and mouse
Authors: Zhang Jintao , He Xiaojin , Wu Huan , Zhang Xin , Yang Shenmin , Liu Chunyu , Liu Siyu , Hua Rong , Zhou Shushu , Zhao Shuqin , Hu Fan , Zhang Junqiang , Liu Wangjie , Cheng Huiru , Gao Yang , Zhang Feng , Cao Yunxia , Liu Mingxi 
Published: June 2021

Abstract
Motile cilia and flagellar defects can result in primary ciliary dyskinesia, which is a multisystemic genetic disorder that affects roughly 1:10 000 individuals. The nexin-dynein regulatory complex (N-DRC) links neighboring doublet microtubules within flagella, serving as a central regulatory hub for motility in Chlamydomonas. Herein, we identified two homozygous DRC1 variants in human patients that were associated with multiple morphological abnormalities of the sperm flagella (MMAF) and male infertility. Drc1−/−, Drc1R554X/R554X and Drc1W244X/W244X mice on the C57BL/6 background suffered from pre-pubertal mortality. However, when the ICR background was introduced, some of these mice were able to survive and recapitulate the MMAF phenotypes detected in human patients. By analyzing these animals, we determined that DRC1 is an essential regulator of N-DRC assembly in cilia and flagella. When DRC1 is absent, this results in the shortening of cilia and consequent impairment of their motility. Damage associated with DRC1 deficiency in sperm flagella was more pronounced than in cilia, as manifested by complete axoneme structural disorder in addition to the loss of the DRC structure. Altogether, these findings suggest that DRC1 is required for the structural stability of flagella but not cilia, emphasizing the key role of this protein in mammalian species.
Quantitative Reduction Theory and Unlikely Intersections
Authors: Daw Christopher , Orr Martin 
Published: June 2021

AbstractWe prove quantitative versions of Borel and Harish-Chandra’s theorems on reduction theory for arithmetic groups. Firstly, we obtain polynomial bounds on the lengths of reduced integral vectors in any rational representation of a reductive group. Secondly, we obtain polynomial bounds in the construction of fundamental sets for arithmetic subgroups of reductive groups, as the latter vary in a real conjugacy class of subgroups of a fixed reductive group. Our results allow us to apply the Pila–Zannier strategy to the Zilber–Pink conjecture for the moduli space of principally polarised abelian surfaces. Building on our previous paper, we prove this conjecture under a Galois orbits hypothesis. Finally, we establish the Galois orbits hypothesis for points corresponding to abelian surfaces with quaternionic multiplication, under certain geometric conditions.
Safety and Tolerability of Mosquito Bite-Induced Controlled Human Infection with Plasmodium vivax in Malaria-Naive Study Participants—Clinical Profile and Utility of Molecular Diagnostic Methods
Authors: Kamau Edwin , Bennett Jason W , Yadava Anjali 
Published: June 2021

Abstract

Background
Plasmodium vivax controlled human malaria infection (PvCHMI) is an important tool for evaluation of drugs, vaccines, and pathologies associated with this parasite. However, there are few data on safety due to limited numbers of PvCHMIs performed.

Methods
We report clinical and laboratory data, including hematological and biochemical profiles and adverse events (AEs), following mosquito bite-induced PvCHMI in malaria-naive study participants. Malaria diagnosis and treatment initiation was based on microscopic analysis of Giemsa-stained slides. Exploratory molecular assays were used to detect parasites using real-time polymerase chain reaction (PCR).

Results
AEs were mild to moderate and no study-related severe AEs were observed in any study participants. The majority of symptoms were transient, resolving within 48 hours. Molecular diagnostic methods detected parasitemia in 100% of study participants before malaria diagnosis using microscopy. Of reported AEs, microscopy detected 67%–100%, quantitative PCR 79%–100%, and quantitative real-time reverse-transcription PCR 96%–100% of study participants prior to appearance of symptoms. Almost all symptoms appeared after initiation of treatment, likely as known consequence of drug treatment.

Conclusions
PvCHMI is safe with the majority of infections being detected prior to appearance of clinical symptoms, which can be further alleviated by using sensitive molecular methods for clinical diagnosis.
Clinical Trials Registration. NCT01157897.
A perspective on cell proliferation kinetics in the root apical meristem
Authors: Desvoyes Bénédicte , Echevarría Clara , Gutierrez Crisanto 
Published: June 2021

Abstract
Organogenesis in plants is primarily postembryonic and relies on a strict balance between cell division and cell expansion. The root is a particularly well-suited model to study cell proliferation in detail since the two processes are spatially and temporally separated for all the different tissues. In addition, the root is amenable to detailed microscopic analysis to identify cells progressing through the cell cycle. While it is clear that cell proliferation activity is restricted to the root apical meristem (RAM), understanding cell proliferation kinetics and identifying its parameters have required much effort over many years. Here, we review the main concepts, experimental settings, and findings aimed at obtaining a detailed knowledge of how cells proliferate within the RAM. The combination of novel tools, experimental strategies, and mathematical models has contributed to our current view of cell proliferation in the RAM. We also discuss several lines of research that need to be explored in the future.
Chlorine-bearing species and the 37Cl/35Cl isotope ratio in the coma of comet 67P/Churyumov–Gerasimenko
Authors: Dhooghe Frederik , De Keyser Johan , Hänni Nora , Altwegg Kathrin , Cessateur Gaël , Jehin Emmanuel , Maggiolo Romain , Rubin Martin , Wurz Peter 
Published: June 2021

ABSTRACT
A full-mission analysis has been conducted of Cl-bearing species in the coma of comet 67P/Churyumov–Gerasimenko as detected by the Double Focusing Mass Spectrometer (DFMS) of Rosetta's ROSINA instrument. The isotope ratio of the two stable chlorine isotopes 37Cl/35Cl is found to be 0.336 ± 0.017, to be compared with the standard mean ocean chloride value of 0.320. The isotope ratio does not change appreciably throughout the mission. The Cl-bearing species fingerprint in DFMS indicates that there is at least one additional chlorine-bearing species in the coma next to HCl, CH3Cl, and NH4Cl. The identity of this volatile or semivolatile species is unknown at this time.
Spectropolarimetry of NGC 3783 and Mrk 509: Evidence for powerful nuclear winds in Seyfert 1 Galaxies
Authors: Lira P , Kishimoto M , Goosmann R W , Campos R , Axon D , Elvis M , Lawrence A , Peterson B M , Robinson A 
Published: June 2021

ABSTRACT
We present results from high signal-to-noise optical spectropolarimetric observations of the Seyfert 1 galaxies NGC 3783 and Mrk 509 in the 3500–7000 Å range. We find complex structure in the polarized emission for both objects. In particular, Position Angle (PA) changes across the Balmer lines show a distinctive ‘M’-shaped profile that had not been observed in this detail before, but could represent a common trait in Seyfert 1 galaxies. In fact, while this shape is observed in all Balmer lines in NGC 3783, Mrk 509 transitions into a ‘M’-shaped PA profile for higher transitions lines. We have modelled the observed profiles using the STOKES radiative transfer code and assuming that the scattering region is co-spatial with the BLR and outflowing. The results give compelling new evidence for the presence of nuclear winds in these two Seyfert 1 galaxies.
Planetary magnetosphere evolution around post-main-sequence stars
Authors: Veras Dimitri , Vidotto Aline A 
Published: June 2021

ABSTRACT
Accompanying the mounting detections of planets orbiting white dwarfs and giant stars are questions about their physical history and evolution, particularly regarding detectability of their atmospheres and potential for habitability. Here we determine how the size of planetary magnetospheres evolves over time from the end of the main sequence through to the white dwarf phase due to the violent winds of red giant and asymptotic giant branch stars. By using a semi-analytic prescription, we investigate the entire relevant phase space of planet type, planet orbit, and stellar host mass ($1\!-\!7\, {\rm M}_{\odot }$). We find that a planetary magnetosphere will always be quashed at some point during the giant branch phases unless the planet’s magnetic field strength is at least two orders of magnitude higher than Jupiter’s current value. We also show that the time variation of the stellar wind and density generates a net increase in wind ram pressure and does not allow a magnetosphere to be maintained at any time for field strengths less than 10−5 T (0.1 G). This lack of protection hints that currently potentially habitable planets orbiting white dwarfs would have been previously inhospitable.
The future influence of six exoplanets on the envelope properties of their parent stars on the giant branches
Authors: Rapoport Ivan , Bear Ealeal , Soker Noam 
Published: June 2021

ABSTRACT
We study the evolution of six exoplanetary systems with the stellar evolutionary code Modules for Experiments in Stellar Astrophysics(mesa) and conclude that they will likely spin-up the envelope of their parent stars on the red giant branch (RGB) or later on the asymptotic giant branch (AGB) to the degree that the mass-loss process might become non-spherical. We choose six observed exoplanetary systems where the semimajor axis is $a_i \simeq 1\small{-}2 {~\rm au}$, and use the binary mode of mesa to follow the evolution of the systems. In four systems, the star engulfs the planet on the RGB, and in two systems on the AGB, and the systems enter a common envelope evolution (CEE). In two systems where the exoplanet masses are Mp ≃ 10MJ, where MJ is Jupiter mass, the planet spins up the envelope to about $10{{\ \rm per\ cent}}$ of the break-up velocity. Such envelopes are likely to have significant non-spherical mass-loss geometry. In the other four systems where Mp ≃ MJ the planet spins up the envelope to values of $1{-}2 {{\ \rm per\ cent}}$ of break-up velocity. Magnetic activity in the envelope that influences dust formation might lead to a small departure from spherical mass-loss even in these cases. In the two cases of CEE on the AGB, the planet deposits energy to the envelope that amounts to ${\gt}10{{\ \rm per\ cent}}$ of the envelope binding energy. We expect this to cause a non-spherical mass-loss that will shape an elliptical planetary nebula in each case.
Molecular line signatures of cloud–cloud collisions
Authors: Priestley F D , Whitworth A P 
Published: June 2021

ABSTRACT
Collisions between interstellar gas clouds are potentially an important mechanism for triggering star formation. This is because they are able to rapidly generate large masses of dense gas. Observationally, cloud collisions are often identified in position–velocity (PV) space through bridging features between intensity peaks, usually of CO emission. Using a combination of hydrodynamical simulations, time-dependent chemistry, and radiative transfer, we produce synthetic molecular line observations of overlapping clouds that are genuinely colliding, and overlapping clouds that are just chance superpositions. Molecules tracing denser material than CO, such as NH3 and HCN, reach peak intensity ratios of 0.5 and 0.2 with respect to CO in the ‘bridging feature’ region of PV space for genuinely colliding clouds. For overlapping clouds that are just chance superpositions, the peak NH3 and HCN intensities are co-located with the CO intensity peaks. This represents a way of confirming cloud collisions observationally and distinguishing them from chance alignments of unrelated material.
Exploiting timing capabilities of the CHEOPS mission with warm-Jupiter planets
Authors: Borsato L , Piotto G , Gandolfi D , Nascimbeni V , Lacedelli G , Marzari F , Billot N , Maxted P F L , Sousa S , Cameron A C , Bonfanti A , Wilson T G , Serrano L M , Garai Z , Alibert Y , Alonso R , Asquier J , Bárczy T , Bandy T , Barrado D , Barros S C C , Baumjohann W , Beck M , Beck T , Benz W , Bonfils X , Brandeker A , Broeg C , Cabrera J , Charnoz S , Csizmadia S , Davies M B , Deleuil M , Delrez L , Demangeon O , Demory B-O , des Etangs A L , Ehrenreich D , Erikson A , Escudé G A , Fortier A , Fossati L , Fridlund M , Gillon M , Guedel M , Hasiba J , Heng K , Hoyer S , Isaak K G , Kiss L , Kopp E , Laskar J , Lendl M , Lovis C , Magrin D , Munari M , Olofsson G , Ottensamer R , Pagano I , Pallé E , Peter G , Pollacco D , Queloz D , Ragazzoni R , Rando N , Rauer H , Ribas I , Ségransan D , Santos N C , Scandariato G , Simon A , Smith A M S , Steller M , Szabó G , Thomas N , Udry S , Van Grootel V , Walton N 
Published: June 2021

ABSTRACT
We present 17 transit light curves of seven known warm-Jupiters observed with the CHaracterising ExOPlanet Satellite (CHEOPS). The light curves have been collected as part of the CHEOPS Guaranteed Time Observation (GTO) program that searches for transit-timing variation (TTV) of warm-Jupiters induced by a possible external perturber to shed light on the evolution path of such planetary systems. We describe the CHEOPS observation process, from the planning to the data analysis. In this work, we focused on the timing performance of CHEOPS, the impact of the sampling of the transit phases, and the improvement we can obtain by combining multiple transits together. We reached the highest precision on the transit time of about 13–16 s for the brightest target (WASP-38, G = 9.2) in our sample. From the combined analysis of multiple transits of fainter targets with G ≥ 11, we obtained a timing precision of ∼2 min. Additional observations with CHEOPS, covering a longer temporal baseline, will further improve the precision on the transit times and will allow us to detect possible TTV signals induced by an external perturber.
Jeans modelling of axisymmetric galaxies with multiple stellar populations
Authors: Caravita Caterina , Ciotti Luca , Pellegrini Silvia 
Published: June 2021

ABSTRACTWe present the theoretical framework to efficiently solve the Jeans equations for multicomponent axisymmetric stellar systems, focusing on the scaling of all quantities entering them. The models may include an arbitrary number of stellar distributions, a dark matter halo, and a central supermassive black hole; each stellar distribution is implicitly described by a two- or three-integral distribution function, and the stellar components can have different structural (density profile, flattening, mass, scale length), dynamical (rotation, velocity dispersion anisotropy), and population (age, metallicity, initial mass function, mass-to-light ratio) properties. In order to determine the ordered rotational velocity and the azimuthal velocity dispersion fields of each component, we introduce a decomposition that can be used when the commonly adopted Satoh decomposition cannot be applied. The scheme developed is particularly suitable for a numerical implementation; we describe its realization within our code JASMINE2, optimized to maximally exploit the scalings allowed by the Poisson and the Jeans equations, also in the post-processing procedures. As applications, we illustrate the building of three multicomponent galaxy models with two distinct stellar populations, a central black hole, and a dark matter halo; we also study the solution of the Jeans equations for an exponential thick disc, and for its multicomponent representation as the superposition of three Miyamoto–Nagai discs. A useful general formula for the numerical evaluation of the gravitational potential of factorized thick discs is finally given.
Comment on ‘An efficient code to solve the Kepler equation: elliptic case’
Authors: Tommasini D , Olivieri D N 
Published: June 2021

ABSTRACTIn a recent MNRAS article, Raposo-Pulido and Pelaez (RPP) designed a scheme for obtaining very close seeds for solving the elliptic Kepler equation with the classical and modified Newton–Raphson methods. This implied an important reduction in the number of iterations needed to reach a given accuracy. However, RPP also made strong claims about the errors of their method that are incorrect. In particular, they claim that their accuracy can always reach the level of ∼5ε, where ε is the machine epsilon (e.g. ε = 2.2 × 10−16 in double precision), and that this result is attained for all values of the eccentricity e &lt; 1 and the mean anomaly M ∈ [0, π], including for e and M that are arbitrarily close to 1 and 0, respectively. However, we demonstrate both numerically and analytically that any implementation of the classical or modified Newton–Raphson methods for Kepler’s equation, including those described by RPP, has a limiting accuracy of the order of ${\sim}\varepsilon /\sqrt{2(1-e)}$. Therefore the errors of these implementations diverge in the limit e → 1, and differ dramatically from the incorrect results given by RPP. Despite these shortcomings, the RPP method can provide a very efficient option for reaching such limiting accuracy. We also provide a limit that is valid for the accuracy of any algorithm for solving Kepler equation, including schemes like bisection that do not use derivatives. Moreover, similar results are also demonstrated for the hyperbolic Kepler equation. The methods described in this work can provide guidelines for designing more accurate solutions of the elliptic and hyperbolic Kepler equations.
A three-dimensional hydrodynamics simulation of oxygen-shell burning in the final evolution of a fast-rotating massive star
Authors: Yoshida Takashi , Takiwaki Tomoya , Aguilera-Dena David R , Kotake Kei , Takahashi Koh , Nakamura Ko , Umeda Hideyuki , Langer Norbert 
Published: June 2021

ABSTRACT
We perform for the first time a 3D hydrodynamics simulation of the evolution of the last minutes pre-collapse of the oxygen shell of a fast-rotating massive star. This star has an initial mass of 38 M⊙, a metallicity of ∼1/50 Z⊙, an initial rotational velocity of 600 km s−1, and experiences chemically homogeneous evolution. It has a silicon- and oxygen-rich (Si/O) convective layer at (4.7–17) × 108 cm, where oxygen-shell burning takes place. The power spectrum analysis of the turbulent velocity indicates the dominance of the large-scale mode (ℓ ∼ 3), which has also been seen in non-rotating stars that have a wide Si/O layer. Spiral arm structures of density and silicon-enriched material produced by oxygen-shell burning appear in the equatorial plane of the Si/O shell. Non-axisymmetric, large-scale (m ≤ 3) modes are dominant in these structures. The spiral arm structures have not been identified in previous non-rotating 3D pre-supernova models. Governed by such a convection pattern, the angle-averaged specific angular momentum becomes constant in the Si/O convective layer, which is not considered in spherically symmetrical stellar evolution models. Such spiral arms and constant specific angular momentum might affect the ensuing explosion or implosion of the star.