bluuebunny/crossref_metadata_2025_split huggingface dataset:
The Effects of Three-dimensional Radiative Transfer on the Resonance Polarization of the Ca i 4227 Å Line
Authors: Jaume Bestard J. , Trujillo Bueno J. , Štěpán J. , del Pino Alemán T. 
Published: March 2021

Abstract
The sizable linear polarization signals produced by the scattering of anisotropic radiation in the core of the Ca i 4227 Å line constitute an important observable for probing the inhomogeneous and dynamic plasma of the lower solar chromosphere. Here we show the results of a three-dimensional (3D) radiative transfer complete frequency redistribution investigation of the line’s scattering polarization in a magnetohydrodynamical 3D model of the solar atmosphere. We take into account not only the Hanle effect produced by the model’s magnetic field but also the symmetry breaking caused by the horizontal inhomogeneities and macroscopic velocity gradients. The spatial gradients of the horizontal components of the macroscopic velocities produce very significant forward scattering polarization signals without the need of magnetic fields, while the Hanle effect tends to depolarize them at the locations where the model’s magnetic field is stronger than about 5 G. The standard 1.5D approximation is found to be unsuitable for understanding the line’s scattering polarization, but we introduce a novel improvement to this approximation that produces results in qualitative agreement with the full 3D results. The instrumental degradation of the calculated polarization signals is also investigated, showing what we can expect to observe with the Visible Spectro-Polarimeter at the upcoming Daniel K. Inouye Solar Telescope.
Revisited Cold Gas Content with Atomic Carbon [C i] in z = 2.5 Protocluster Galaxies
Authors: Lee Minju M. , Tanaka Ichi , Iono Daisuke , Kawabe Ryohei , Kodama Tadayuki , Kohno Kotaro , Saito Toshiki , Tamura Yoichi 
Published: March 2021

Abstract
We revisit the cold gas contents of galaxies in a protocluster at z = 2.49 using the lowest neutral atomic carbon transition [C i] 3
P
1 − 3
P
0 from Atacama Large Millimeter/submillimeter Array observations. We aim to test if the same gas-mass calibration adopted in field galaxies can be applied to protocluster galaxies. Five galaxies out of 16 targeted galaxies are detected in the [C i] line, and these are all previously detected in CO (3–2) and CO (4–3) and three in 1.1 mm dust continuum. We investigate the line luminosity relations between CO and [C i] in the protocluster and compare with other previous studies. We then compare the gas mass based on three gas tracers of [C i], CO(3–2), and dust if at least one of the last two tracers are available. Using the calibration adopted for field main-sequence galaxies, the [C i]-based gas measurements are lower than or comparable to the CO-based gas measurements by −0.35 dex at the lowest with the mean deviation of −0.14 dex. The differences between [C i]- and the dust- based measurements are relatively mild by up to 0.16 dex with the mean difference of 0.02 dex. Taking these all together with calibration uncertainties, with the [C i] line, we reconfirm our previous findings that the mean gas fraction is comparable to field galaxies for a stellar-mass range of

. However, at least for these secure five detections, the depletion timescale decreases more rapidly with stellar mass than field galaxies that might be related to earlier quenching in dense environments.
A Complex Luminosity Function for the Anomalous Globular Clusters in NGC 1052-DF2 and NGC 1052-DF4
Authors: Shen Zili , van Dokkum Pieter , Danieli Shany 
Published: March 2021

Abstract
NGC 1052-DF2 and NGC 1052-DF4 are ultradiffuse galaxies that have extremely low velocity dispersions, indicating that they have little or no dark matter. Both galaxies host anomalously luminous globular clusters (GCs), with a peak magnitude of their GC luminosity function (GCLF) that is ∼1.5 mag brighter than the near-universal value of M

V
≈ −7.5. Here we present an analysis of the joint GCLF of the two galaxies, making use of new Hubble Space Telescope photometry and Keck spectroscopy and a recently improved distance measurement. We apply a homogeneous photometric selection method to the combined GC sample of DF2 and DF4. The new analysis shows that the peak of the combined GCLF remains at M

V
≈ −9 mag. In addition, we find a subpopulation of less luminous GCs at M

V
≈ −7.5 mag, where the near-universal GCLF peak is located. The number of GCs in the magnitude range of −5 to −8 is

in DF2 and

in DF4, similar to that expected from other galaxies of the same luminosity. The total GC number between M

V
of −5 and −11 is

for DF2 and

for DF4, calculated from the background-subtracted GCLF. The data are consistent with both galaxies having two GC populations: the one expected for their luminosity, and a very luminous population composing ∼90% of the total cluster mass. The number of GCs does not scale with the halo mass in either DF2 or DF4, suggesting that N
GC is not directly determined by the merging of halos.
ALMA Observations of Massive Clouds in the Central Molecular Zone: Ubiquitous Protostellar Outflows
Authors: Lu 吕 Xing 行 , Li Shanghuo , Ginsburg Adam , Longmore Steven N. , Kruijssen J. M. Diederik , Walker Daniel L. , Feng Siyi , Zhang Qizhou , Battersby Cara , Pillai Thushara , Mills Elisabeth A. C. , Kauffmann Jens , Cheng Yu , Inutsuka Shu-ichiro 
Published: March 2021

Abstract
We observe 1.3 mm spectral lines at 2000 au resolution toward four massive molecular clouds in the Central Molecular Zone (CMZ) of the Galaxy to investigate their star formation activities. We focus on several potential shock tracers that are usually abundant in protostellar outflows, including SiO, SO, CH3OH, H2CO, HC3N, and HNCO. We identify 43 protostellar outflows, including 37 highly likely ones and 6 candidates. The outflows are found toward both known high-mass star-forming cores and less massive, seemingly quiescent cores, while 791 out of the 834 cores identified based on the continuum do not have detected outflows. The outflow masses range from less than 1 M
⊙ to a few tens of M
⊙, with typical uncertainties of a factor of 70. We do not find evidence of disagreement between relative molecular abundances in these outflows and in nearby analogs such as the well-studied L1157 and NGC 7538S outflows. The results suggest that (i) protostellar accretion disks driving outflows ubiquitously exist in the CMZ environment, (ii) the large fraction of candidate starless cores is expected if these clouds are at very early evolutionary phases, with a caveat on the potential incompleteness of the outflows, (iii) high-mass and low-mass star formation is ongoing simultaneously in these clouds, and (iv) current data do not show evidence of a difference between the shock chemistry in the outflows that determines the molecular abundances in the CMZ environment and in nearby clouds.
SN 2017hpa: A Nearby Carbon-rich Type Ia Supernova with a Large Velocity Gradient
Authors: Zeng Xiangyun , Wang Xiaofeng , Esamdin Ali , Pellegrino Craig , Zheng WeiKang , Zhang Jujia , Mo Jun , Li Wenxiong , Howell D. Andrew , Filippenko Alexei V. , Lin Han , Brink Thomas G. , Baron Edward A. , Burke Jamison , DerKacy James M. , McCully Curtis , Hiramatsu Daichi , Hosseinzadeh Griffin , Jeffers Benjamin T. , Ross Timothy W. , Stahl Benjamin E. , Stegman Samantha , Valenti Stefano , Wang Lifan , Xiang Danfeng , Zhang Jicheng , Zhang Tianmeng 
Published: March 2021

Abstract
We present extensive, well-sampled optical and ultraviolet photometry and optical spectra of the Type Ia supernova (SN Ia) 2017hpa. The light curves indicate that SN 2017hpa is a normal SN Ia with an absolute peak magnitude of

−19.12 ± 0.11 mag and a postpeak decline rate Δm
15(B) = 1.02 ± 0.07 mag. According to the quasi-bolometric light curve, we derive a peak luminosity of 1.25 × 1043 erg s−1 and a 56Ni mass of 0.63 ± 0.02 M
⊙. The spectral evolution of SN 2017hpa is similar to that of normal Ia supernovae (SNe Ia), while it exhibits an unusually rapid velocity evolution resembling that of SN 1991bg-like SNe Ia or the high-velocity subclass of SNe Ia, with a postpeak velocity gradient of ∼130 ± 7 km s−1 day−1. Moreover, its early spectra (t < − 7.9 days) show a prominent C ii
λ6580 absorption feature, which disappeared in near-maximum-light spectra but reemerged at phases from t ∼ + 8.7 days to t ∼ + 11.7 days after maximum light. This implies that some unburned carbon may mix deep into the inner layer and is supported by the low C ii
λ6580-to-Si ii
λ6355 velocity ratio (∼0.81) observed in SN 2017hpa. The O i
λ7774 line shows a velocity distribution like that of carbon. The prominent carbon feature, the low velocity seen in carbon and oxygen, and the large velocity gradient make SN 2017hpa stand out from other normal SNe Ia and are more consistent with predictions from a violent merger of two white dwarfs. Detailed modeling is still needed to reveal the nature of SN 2017hpa.
Effects of Forcing Mechanisms on the Multiscale Properties of Magnetohydrodynamics
Authors: Yang Yan , Linkmann Moritz , Biferale Luca , Wan Minping 
Published: March 2021

Abstract
We performed numerical simulations to study the response of magnetohydrodynamics (MHD) to large-scale stochastic forcing mechanisms parameterized by one parameter, 0 ≤ a ≤ 1, going from direct injection on the velocity field (a = 1) to stirring acts on the magnetic field only (a = 0). We study the multiscale properties of the energy transfer by splitting the total flux in channels mediated by (i) the kinetic nonlinear advection, (ii) the Lorentz force, (iii) the magnetic advection, and (iv) the magnetic stretching term. We further decompose the fluxes into two subchannels given by heterochiral and homochiral components in order to distinguish forward, inverse, and flux-loop cascades. We show that there exists a quasi-singular role of the magnetic forcing mechanism for a ∼ 1: a small injection on the magnetic field a < 1 can strongly deplete the mean flux of kinetic energy transfer throughout the kinetic nonlinear advection channel. We also show that this negligible mean flux is the result of a flux-loop balance between heterochiral (direct) and homochiral (inverse) transfers. Conversely, both homochiral and heterochiral channels transfer energy forward for the other three channels. Cross-exchange between velocity and the magnetic field is reversed around a = 0.4, and except when a ∼ 1, we always observe that heterochiral mixed velocity–magnetic energy triads tend to move energy from magnetic to velocity fields. Our study is an attempt to further characterize the multiscale nature of MHD dynamics by disentangling different properties of the total energy transfer mechanisms, which can be useful for improving subgrid modeling.
Oceanic Superrotation on Tidally Locked Planets
Authors: Zeng Yaoxuan , Yang Jun 
Published: March 2021

Abstract
Is there oceanic superrotation on exoplanets? Atmospheric superrotation, characterized by west-to-east winds over the equator, is a common phenomenon in the atmospheres of Venus, Titan, Saturn, Jupiter, and tidally locked exoplanets. The stratospheric atmosphere of Earth is also superrotating during the westerly phase of the quasi-biennial oscillation. However, whether the same phenomenon can occur in the ocean is poorly known. Through numerical simulations, here we show that oceanic superrotation does occur on tidally locked terrestrial planets around low-mass stars. Its formation (spun up from rest) is associated with surface winds, the equatorward momentum convergence by Rossby waves, and the eastward propagation of Kelvin waves in the ocean. Its maintenance is driven by equatorward momentum transports of coupled Rossby–Kelvin waves in the ocean excited from the uneven stellar radiation distribution. The width of the superrotation is mainly constrained by the Rossby deformation radius in the ocean, while its strength is more complex. Many factors can influence the strength, including planetary rotation rate, stellar flux, greenhouse gas concentration, seawater salinity, and bottom drag, but a scaling theory for the strength of the oceanic superrotation is lacking. This work confirms that oceanic superrotation can occur on tidally locked terrestrial planets with seawater oceans and suggests that it may also occur on tidally locked hot planets with magma oceans that will possibly be observed in the near future.
New Bistable Solutions in Molecular Cloud Chemistry: Nitrogen and Carbon Autocatalysis
Authors: Dufour Gwenaëlle , Charnley Steven B. 
Published: March 2021

Abstract
We have investigated the chemistry of dense interstellar clouds and found new bistable solutions in the nitrogen and carbon chemistries. We identify the autocatalytic processes that are present in the pure, reduced, chemical networks and find, as previously found for oxygen chemistry, that He+ plays an important role. The applicability of these results to astronomical environments is briefly discussed. The bistable solutions found for carbon chemistry occur for low densities and high ionization fractions that are not compatible with those found in cold, dense clouds. Bistability in the pure nitrogen chemistry occurs for conditions that are relevant for prestellar cores in which significant CO depletion has taken place. We conclude that several autocatalyses are embedded in gas-phase interstellar chemistry and that many more are potentially present.
DNA barcodes from northern birds of Colombia
Authors: Pulgarín-R Paulo , Olivera-Angel Martha , Ortíz Luisa , Nanclares Duván , Velásquez-Restrepo Sara , Diaz-Nieto Juan 
Published: March 2021

DNA barcode datasets are a useful tool for conservation and aid in taxonomic identification, particularly in megadiverse tropical countries seeking to document and describe its biota, which is dropping at an alarming rate during recent decades. Here we report the barcodes for several low elevation bird species from northern Colombia with the goal to provide tools for species identification in this region of South America. We blood sampled birds in a lowland tropical forest with various degrees of intervention using standard 10 × 12 mist-nets. We extracted DNA and sequenced the COI barcode gene using standard primers and laboratory methods. We obtained 28 COI sequences from 19 species, 10 families and 3 orders and found that barcodes largely matched (but not always) phenotypic identification (>90%) and they also facilitated the identification of several challenging passerine species. Despite our reduced sampling, our study represents the first attempt to document COI barcodes for birds (from blood samples) in this part of Colombia, which fills a considerable gap of sampling in this part of South America.
Le faux-self familial
Authors: Tordo Frédéric 
Published: March 2021

Le faux-self familial apparaît comme une organisation fondamentale de la famille, qui présente alors une identité de surface, ou une fausse identité. Ses caractéristiques sont les suivantes : le faux-self familial est un phénomène groupal, qui concerne les membres d’une famille ; il se traduit par l’impossibilité de convoquer une pensée réflexive familiale ; pour tenter de se défaire d’une souffrance, ou d’une toxicité dans les liens, l’organisation familiale poursuit une extinction de la résonance fantasmatique ; pour faire écran à cette vitalité perdue, la famille peut s’accrocher à un objet en lien qui offre à ses membres l’illusion d’une dynamique ; en conséquence, la famille met en place une idéologie artificielle, qui artificialise en retour les liens familiaux.
Violence et défaut de rêverie dans le couple
Authors: Sanahuja Maria de la Almudena , Bernard Alexandra , Naimi Marie 
Published: March 2021

Les situations de violences conjugales sont de plus en plus visibles dans l’espace sociétal, politique. Elles s’invitent également dans l’intimité de la scène thérapeutique. L’esquisse d’un modèle de compréhension de la violence dans le couple, en appui sur la théorie analytique familiale, nous conduit à formuler l’hypothèse d’une « empreinte inconsciente maudite », venin transgénérationnel déployé dans l’enveloppe psychique contenant les partenaires. Ce phénomène a pour effet l’abrasion de la capacité de rêverie du couple (« inrêverie couplale »).
Collagen Fibril Abnormalities in the Extraocular Muscles in Ehlers-Danlos Syndrome
Authors: Meyer Ewy , Ludatscher Ruth M , Zonis Shlomo 
Published: March 2021

ABSTRACT
The dermal collagen fibrils and the fibrils of the extraocular muscles and the conjunctivas of both eyes of a child afflicted with Ehlers-Danlos syndrome (EDS) were studied ultrastructurally. The results were evaluated statistically. Biopsy material was used In all Instances. The collagen fibrils from all involved tissues showed a high percentage of size variation. Abnormalities of shape were noted. In the reticular dermis, 48% of fibrils were of normal diameter, 23% were enlarged, and 29% were thinner than normal. In the extraocular muscles, 77% were of normal size, 14.5% were larger, and 8.5% were smaller. In the conjunctivas, 73% of fibrils were normal-sized, 22% were enlarged, and 5% were of small diameter. No small-sized fibrils were encountered in control extraocular muscles.
Experience in Identifying the Variant Adrenal Venous anatomy during Modified Retroperitoneoscopic Adrenalectomy
Authors: Hu Dongliang , Zhu Dan , Zhang Yingao , Wang Xinghuan 
Published: March 2021

Background:
Adrenal vein plays an important role in performing laparoscopic adrenalectomy successfully. However, it often presents with a multitude of venous anatomical variants. Hence, having a thorough knowledge on the variant types is crucial to reduce operative complications. This study aims to present our experience in identifying adrenal vein variation in adrenalectomy through modified retroperitoneal approach.

Patients and Methods:
A total of 187 patients underwent modified retroperitoneoscopic adrenalectomy between July 2017 and February 2019. Perioperative data and adrenal vein variants were recorded and analysed.

Results:
Variant adrenal veins were encountered in seven patients. On the right side, two cases were drained by two adrenal veins; one case had a common trunk of adrenal vein and an accessory hepatic vein and one case had an adrenal vein joined with the opening of the right renal vein. On the left side, two cases of anatomic variations were described as follows: one vein converged with the left inferior phrenic vein and joined with the left renal vein, whereas the other vein directly joined with the left renal vein. One case had two adrenal veins that joined with the left renal vein.

Conclusions:
Accurate identification and proper handling of the anatomical variation in the drainage of adrenal vein are crucial to safe LA. It is helpful to anticipate and avoid bleeding, especially in large adrenal tumours.
Prevalence of dental fear in children of 3–14 years visiting the OPD in Dental College, Lucknow, India
Authors: Singh Ankita , Palshikar Anuradha , Agarwal Sugandha , Singh Shweta 
Published: March 2021

Introduction:
Dental fear and anxiety pose a significant problem for the practice of dentistry, especially in children. Therefore, it is necessary to identify and quantify this anxiety, to implement, and to monitor the effectiveness of treatment interventions.

Materials and Methods:
A cross-sectional study was conducted on children in the age group of 3–14 years. The children who had sound health and visited outpatient department of a Dental College, Lucknow, India with their parents for dental care were considered for study purposes. Children’s dental fear and anxiety were measured by using three scales.

Result:
Out of the total 220 respondents, 118 (53.6%) were males and 102 (46.4%) females. The outcome of the study showed that the dental fear among children was 13.3%, 22.9%, 7.8%, respectively, in existence measured by the three scales, viz., (a) facial image scale (FIS), (b) dental fear scale (DFS), and (c) children’s fear survey schedule-dental subscale (CFSS-DS). About 70.2% of the children showed Frankl’s behavior rating of 3, i.e. positive.

Conclusion:
Dental fear and anxiety are the most common problems of children and because of this, they are afraid of undergoing any dental treatment. By using the above scale, we can know about those factors which can enhance their fear so that we can modify our treatment approach. Altering in a treatment modality not only leads the children to get the treatment done easily but also removes the fear for dental treatment in the future.
Cross-sectional study regarding pattern of adverse drug reactions in a tertiary care hospital, Kakinada, India
Authors: Bendi Sreenivasa Rao , Suvvari Tarun Kumar , Kutikuppala Lakshmi Venkata Simhachalam 
Published: March 2021

Introduction:
Drugs are considered as double-edged weapons with the potential to cause benefit as well as harm. Recent studies reveal that adverse drug reactions (ADRs) imply a remarkable burden on the length of hospital stay, healthcare facilities, and sometimes they require additional investigations and drug therapies for the treatment of symptoms and diseases caused to the patient. So, further local studies are required to understand the scenario and to improve the safety of prescribing and monitoring drugs and improved patient adherence to medication.

Objectives:
To evaluate and assess the pattern of adverse drug reactions reported to the ADR Monitoring Centre, Rangaraya Medical College, Kakinada, India.

Materials and Methods:
The current study was a retrospective and an observational type of study carried out at the ADR Monitoring Centre of a tertiary care hospital. Total ADRs reported during the two years from June 2016 to June 2018 were included in the study. Each ADR was analyzed for demographic data, relationship to drugs as per causality assessment, and frequency of ADRs. Microsoft Excel 2019 and SPPS version 20 were used for data analysis.

Results:
The most common group of drugs showing ADRs were anti-retroviral therapy (ART) drugs, followed by anti-microbial agents. Most of the ADRs were probable and mild. Rash was the most frequently occurring ADR.

Conclusion:
The study of ADRs in a particular institute using demographic patterns will contribute to patient safety by sensitizing the clinicians in that particular institute.