bluuebunny/crossref_metadata_2025_split huggingface dataset:
Changing “portrait” of patients with newly diagnosed idiopathic pulmonary hypertension over the past two decades
Authors: Shariya A. M. , Martynyuk T. V. 
Published: October 2024

Objective: to perform a comprehensive analysis of the clinical, functional and hemodynamic status of patients with idiopathic pulmonary hypertension (IPAH) to compare the "portrait" of historical and modern subgroups. Materials and methods. The study included 120 patients with IPAH observed in the Department of Pulmonary Hypertension and Heart Diseases, E.I. Chazov National Medical Research Center of Cardiology. The pts were divided into 2 subgroups depending on the time of diagnosis and were comparable in terms of the initial functional class (WHO). A comparative analysis of clinical, functional, and hemodynamic parameters was carried out. The diagnosis was established according to the algorithm of the Eurasian (2019) and Russian guidelines for the diagnosis and treatment of pulmonary hypertension (PH) (2020). Results. The median time from the onset of PH symptoms to diagnosis in the historical and modern cohorts was 24 months and 13.5 months, respectively, and from the first visit to the diagnosis of IPAH – 13 months and 3.5 months. The median age of patients was 31 years and 40.5 years. In both subgroups, the number of women dominated – up to 86.6 % of patients in the modern cohort. Clinical, laboratory, functional and instrumental tests did not differ significantly between the subgroups. In the structure of concomitant pathology, comorbidity with cardiovascular pathology is most common, in a larger percentage in the modern cohort of patients: hypertension – up to 31.6 %, obesity – up to 25 % and diabetes mellitus – up to 5 %. According to various risk assessment scales, most patients in both subgroups demonstrated intermediate risk at the time of diagnosis, but in the modern cohort, a large proportion of high-risk patients was noted (20.0 %). Conclusion. Nowadays, IPAH remains a late-diagnosed disease, which contributes to a later treatment prescription. The clinical "portrait" of patients with IPAH has changed over the years towards older and more comorbid patients, especially with cardiovascular diseases. Timely detection and treatment of concomitant pathology, timely risk assessment are the key to prescribing the most effective treatment regimens, improving the quality of life and prognosis of patients with IPAH.
Eurasian Association of Cardiology (EAC)/ Russian society of somnologists (RSS) guidelines for the diagnosis and treatment of obstructive sleep apnea in patients with cardiovascular diseases (2024)
Authors: Litvin A. Yu. , Chazova I. E. , Elfimova E. M. , Pevzner A. V. , Poluektov M. G. , Danilov N. M. , Mikhailova O. O. , Aksenova A. V. 
Published: October 2024

The aim of this guideline is to assist physicians in the management of patients with cardiovascular pathology and obstructive sleep-disordered breathing. The article consists data on diagnostic tactics for patients with possible sleep-breathing disorders, describes the basic principles of obstructive sleep apnea treatment, and substantiates the clinical significance of obstructive sleep apnea therapy initiating in the management of patients with cardiovascular diseases.
Magnetic resonance and computed tomography in patients with arrhythmia after cardiac surgery
Authors: Shlyappo M. A. , Aleksandrova S. A. , Sopov O. V. , Golukhova E. Z. 
Published: October 2024

Progress in the treatment of arrhythmias is associated with the development and implementation in clinical medicine of a number of electrophysiological methods that make it possible to determine and localize the formation and conduction of electrical excitation with a high degree of reliability. At the same time, an increase in the number of invasive procedures can lead to an increase in complications associated with the interventions, which in turn requires radiology specialists to understand the main stages of the intervention technique, and, accordingly, the mechanisms of development of possible complications and their localization. The purpose of the article is to present modern research data on the use of computed and magnetic resonance imaging in determining complications during interventional and surgical treatment of cardiac arrhythmias.
KPF Confirms a Polar Orbit for KELT-18 b
Authors: Rubenzahl Ryan A. , Dai Fei , Halverson Samuel , Howard Andrew W. , Householder Aaron , Fulton Benjamin , Behmard Aida , Gibson Steven R. , Roy Arpita , Shaum Abby P. , Isaacson Howard , Brodheim Max , Deich William , Hill Grant M. , Holden Bradford , Laher Russ R. , Lanclos Kyle , Payne Joel N. , Petigura Erik A. , Schwab Christian , Smith Chris , Stefánsson Guðmundur , Walawender Josh , Wang Sharon X. , Weiss Lauren M. , Winn Joshua N. , Wishnow Edward 
Published: October 2024

Abstract
We present the first spectroscopic transit results from the newly commissioned Keck Planet Finder on the Keck-I telescope at W. M. Keck Observatory. We observed a transit of KELT-18 b, an inflated ultrahot Jupiter orbiting a hot star (T
eff = 6670 K) with a binary stellar companion. By modeling the perturbation to the measured cross-correlation functions using the Reloaded Rossiter–McLaughlin technique, we derived a sky-projected obliquity of λ = − 94.°8 ± 0.°7 (

ψ
=

93.8

−
1.8

+
1.6

°

for isotropic i
⋆). The data are consistent with an extreme stellar differential rotation (α = 0.9), though a more likely explanation is moderate center-to-limb variations of the emergent stellar spectrum. We see additional evidence for the latter from line widths increasing toward the limb. Using loose constraints on the stellar rotation period from observed variability in the available TESS photometry, we were able to constrain the stellar inclination and thus the true 3D stellar obliquity to

ψ
=

91.7

−
1.8

+
2.2

°

. KELT-18 b could have obtained its polar orbit through high-eccentricity migration initiated by Kozai–Lidov oscillations induced by the binary stellar companion KELT-18 B, as the two likely have a large mutual inclination as evidenced by Gaia astrometry. KELT-18 b adds another data point to the growing population of close-in polar planets, particularly around hot stars.
JADES Ultrared Flattened Objects: Morphologies and Spatial Gradients in Color and Stellar Populations
Authors: Gibson Justus L. , Nelson Erica , Williams Christina C. , Price Sedona H. , Whitaker Katherine E. , Suess Katherine A. , de Graaff Anna , Johnson Benjamin D. , Bunker Andrew J. , Baker William M. , Bhatawdekar Rachana , Boyett Kristan , Charlot Stephane , Curtis-Lake Emma , Eisenstein Daniel J. , Hainline Kevin , Hausen Ryan , Maiolino Roberto , Rieke George , Rieke Marcia , Robertson Brant , Tacchella Sandro , Willott Chris 
Published: October 2024

Abstract
One of the more surprising findings after the first year of JWST observations is the large number of spatially extended galaxies (ultrared flattened objects, or UFOs) among the optically faint galaxy (OFG) population otherwise thought to be compact. Leveraging the depth and survey area of the JWST Advanced Deep Extragalactic Survey, we extend observations of the OFG population to an additional 112 objects, 56 of which are well-resolved in F444W with effective sizes, R

e
> 0.″25, more than tripling previous UFO counts. These galaxies have redshifts around 2 < z < 4, high stellar masses (

log
(

M

*

/

M

⊙

)
∼
10
–
11

), and star formation rates around ∼100–1000 M
⊙ yr−1. Surprisingly, UFOs are red across their entire extents, which spatially resolved analysis of their stellar populations shows is due to large values of dust attenuation (typically A

V
> 2 mag even at large radii). Morphologically, the majority of our UFO sample tends to have low Sérsic indices (n ∼ 1) suggesting that these large, massive, OFGs have little contribution from a bulge in F444W. Further, a majority have axis ratios between 0.2 < q < 0.4, which Bayesian modeling suggests that their intrinsic shapes are consistent with being a mixture of inclined disks and prolate objects with little to no contribution from spheroids. While kinematic constraints will be needed to determine the true intrinsic shapes of UFOs, it is clear that an unexpected population of large, disky or prolate objects contributes significantly to the population of OFGs.
Plasma Dynamics and Nonthermal Particle Acceleration in 3D Nonrelativistic Magnetic Reconnection
Authors: Zhang Qile , Guo Fan , Daughton William , Li Xiaocan , Li Hui 
Published: October 2024

Abstract
Understanding plasma dynamics and nonthermal particle acceleration in 3D magnetic reconnection has been a long-standing challenge. In this paper, we explore these problems by performing large-scale fully kinetic simulations of multi-X-line plasmoid reconnection with various parameters in both the weak- and strong-guide-field regimes. In each regime, we have identified its unique 3D dynamics that lead to field-line chaos and efficient acceleration, and we have achieved nonthermal acceleration of both electrons and protons into power-law spectra. The spectral indices agree well with a simple Fermi acceleration theory that includes guide-field dependence. In the low-guide-field regime, the flux rope kink instability governs the 3D dynamics for efficient acceleration. The weak dependence of the spectra on the ion-to-electron mass ratio and β (≪1) implies that the particles are sufficiently magnetized for Fermi acceleration in our simulations. While both electrons and protons are injected at reconnection exhausts, protons are primarily injected by perpendicular electric fields through Fermi reflections and electrons are injected by a combination of perpendicular and parallel electric fields. The magnetic power spectra agree with in situ magnetotail observations, and the spectral index may reflect a reconnection-driven size distribution of plasmoids instead of the Goldreich–Sridhar vortex cascade. As the guide field becomes stronger, the oblique flux ropes of large sizes capture the main 3D dynamics for efficient acceleration. Intriguingly, the oblique flux ropes can also experience flux rope kink instability, to drive extra 3D dynamics. This work has broad implications for 3D reconnection dynamics and particle acceleration in heliophysics and astrophysics.
Thermal Fluctuations of Matter Composition and Quark Nucleation in Compact Stars
Authors: Guerrini Mirco , Pagliara Giuseppe , Drago Alessandro , Lavagno Andrea 
Published: October 2024

Abstract
At the extreme densities reached in the core of neutron stars, it is possible that deconfined quark matter is produced. The formation of this new phase of strongly interacting matter is likely to occur via a first-order phase transition for the typical temperatures reached in astrophysical processes. The first seeds of quark matter would then form through a process of nucleation within the metastable hadronic phase. Here, we address the role of the thermal fluctuations in the hadronic composition on the nucleation of two-flavor quark matter. At finite temperature, the thermodynamic quantities in a system fluctuate around average values. Nucleation being a local process, it is possible that it occurs in a subsystem whose composition makes the nucleation easier. We will consider the total probability of the nucleation as the product between the probability that a subsystem has a certain hadronic composition different from the average in the bulk, and the nucleation probability in that subsystem. We will show how those fluctuations of the hadronic composition can increase the efficiency of nucleation already for temperatures ∼(0.1−1) keV. However, for temperatures ≲(1−10) MeV, the needed overpressure exceeds the maximum pressure reached in compact stars. Finally, for even larger temperatures the process of nucleation can take place, even taking into account finite-size effects.
A Data-driven Spectral Model of Main-sequence Stars in Gaia DR3
Authors: Angelo Isabel , Bedell Megan , Petigura Erik , Ness Melissa 
Published: October 2024

Abstract
Precise spectroscopic classification of planet hosts is an important tool of exoplanet research at both the population and individual system level. In the era of large-scale surveys, data-driven methods offer an efficient approach to spectroscopic classification that leverages the fact that a subset of stars in any given survey has stellar properties that are known with high fidelity. Here, we use The Cannon, a data-driven framework for modeling stellar spectra, to train a generative model of spectra from the Gaia Data Release 3 Radial Velocity Spectrometer (RVS). Our model derives stellar labels with precisions of 72 K in T
eff, 0.09 dex in logg, 0.06 dex in [Fe/H], 0.05 dex in [α/Fe], and 1.9 km s−1 in v
broad for main-sequence stars observed by Gaia DR3 by transferring GALAH labels, and is publicly available at https://github.com/isabelangelo/gaiaspec. We validate our model performance on planet hosts with available Gaia RVS spectra at SNR>50 by showing that our model is able to recover stellar parameters at ≥20% improved accuracy over the existing Gaia stellar parameter catalogs, measured by the agreement with high-fidelity labels from the Spectroscopic Observations of Cool Stars survey. We also provide metrics to test for stellar activity, binarity, and reliability of our model outputs and provide instructions for interpreting these metrics. Finally, we publish updated stellar labels and metrics that flag suspected binaries and active stars for Kepler Input Catalog objects with published Gaia RVS spectra.
Mock Observations: Three Different Types of Galaxy Alignment in TNG100 Simulations
Authors: Lan Yanyao , Tang Lin , Lin Weipeng , Gong Junyu 
Published: October 2024

Abstract
In this study, galaxy samples have been generated using mock observation techniques based on the results of TNG100-1 simulations to investigate three forms of intrinsic alignment: satellite-central alignment between the orientation of the brightest group galaxies (BGG) and the spatial distribution of their satellites, radial alignment between the satellites’ orientation and the direction toward their BGG, as well as direct alignment between the orientation of BGG and that of its satellites. Overall, the predictions of galaxy alignment generally align with observations, although minor discrepancies have been identified. For satellite-central alignment, the alignment strength and color-dependence trends are well replicated by the mock observations. Regarding radial alignment, the signals are weak but discernible, with no apparent color dependence. As for direct alignment, no signal is detected, nor is there any color dependence. We also investigate the alignment dependencies on halo or the BGG properties, and proximity effect. For satellite-central alignment, the predicted alignment signal shows a positive correlation with halo and BGG mass, consistent with observations and previous predictions. Similar correlations have also been observed with the BGG age and metallicity, which merit future observational analysis for confirmation. Proximity effects have been observed for all three types of alignment, with satellites closer to the BGG exhibiting stronger alignment signals. The influence of galaxy definition and shape determination on alignment studies is also analyzed. This study underscores the importance of employing mock observation techniques for a fair comparison between predictions and observations.
Electrostatic Waves and Electron Holes in Simulations of Low-Mach Quasi-perpendicular Shocks
Authors: Bohdan Artem , Tran Aaron , Sironi Lorenzo , Wilson Lynn B. 
Published: October 2024

Abstract
Collisionless low-Mach-number shocks are abundant in astrophysical and space plasma environments, exhibiting complex wave activity and wave–particle interactions. In this paper, we present 2D Particle-in-Cell (PIC) simulations of quasi-perpendicular nonrelativistic (v
sh ≈ (5500–22000) km s−1) low-Mach-number shocks, with a specific focus on studying electrostatic waves in the shock ramp and precursor regions. In these shocks, an ion-scale oblique whistler wave creates a configuration with two hot counterstreaming electron beams, which drive unstable electron acoustic waves (EAWs) that can turn into electrostatic solitary waves (ESWs) at the late stage of their evolution. By conducting simulations with periodic boundaries, we show that the EAW properties agree with linear dispersion analysis. The characteristics of ESWs in shock simulations, including their wavelength and amplitude, depend on the shock velocity. When extrapolated to shocks with realistic velocities (v
sh ≈ 300 km s−1), the ESW wavelength is reduced to one-tenth of the electron skin depth and the ESW amplitude is anticipated to surpass that of the quasi-static electric field by more than a factor of 100. These theoretical predictions may explain a discrepancy, between PIC and satellite measurements, in the relative amplitude of high- and low-frequency electric field fluctuations.
Exploring the Central Region of NGC 1365 in the Ultraviolet Domain
Authors: Kurian Kshama Sara , Stalin C. S. , Wylezalek Dominika , Lyubenova Mariya , Adhikari Tek Prasad , Devaraj Ashish , Sagar Ram , Kissler-Patig Markus , Mondal Santanu 
Published: October 2024

Abstract
Active galactic nuclei (AGN) feedback and its impact on their host galaxies are critical to our understanding of galaxy evolution. Here, we present a combined analysis of new high resolution ultraviolet (UV) data from the Ultraviolet Imaging Telescope (UVIT) on AstroSat and archival optical spectroscopic data from the Very Large Telescope/MUSE, for the Seyfert galaxy, NGC 1365. Concentrating on the central 5 kpc region, the UVIT images in the far- and near-UV show bright star-forming knots in the circumnuclear ring as well as a faint central source. After correcting for extinction, we found the star formation rate (SFR) surface density of the circumnuclear 2 kpc ring to be similar to other starbursts, despite the presence of an AGN outflow, as seen in [O iii] 5007 Å. On the other hand, we found fainter UV and thus lower SFR in the direction southeast of the AGN relative to northwest in agreement with observations at other wavelengths from JWST and Atacama Large Millimeter/submillimeter Array. The AGN outflow velocity is found to be lesser than the escape velocity, suggesting that the outflowing gas will rain back into the galaxy. The deep UV data have also revealed diffuse UV emission in the direction of the AGN outflow. By combining [O iii] and UV data, we found the diffuse emission to be of AGN origin.
Causal Attention Deep-learning Model for Solar Flare Forecasting
Authors: Zhang Xinze , Xu Long , Li Zihan , Huang Xin 
Published: October 2024

Abstract
Solar flares originate from the sudden release of energy stored in the magnetic field of the active region on the Sun, but the trigger for flares is still uncertain. Currently, deep-learning-based solar flare prediction models have achieved good results and are widely recognized. However, these models focus more on data correlation rather than causality. An ideal flare prediction model should probe into the causes/triggers of solar flares, and diagnose the precursors of flares rather than just correlation analysis. To extract more informative precursors of flares from magnetograms, while suppressing the interference of confounding factors, a causal attention module is introduced to disentangle causal and confounder features from the input features. To address the problem of imbalanced positive and negative samples in the data set, an adaptive data set split mechanism is proposed. It divides the data set into several balanced subsets of positive and negative samples, and dynamically adjusts the subsets according to the model’s prediction results during the training process. The experimental results demonstrate that our proposed model achieves 4.08%, 8.38%, and 2.19% higher accuracy, true skill score, and area under the receiver operating characteristic curve than the baseline model. Additionally, the class-specific heatmaps by using the gradient-weighted class activation mapping method reveal that our proposed model generally focuses on the polarity inverse line of active regions, well in line with theoretical study.
Validating Gaia DR3 Pulsating Variable Classifications with TESS. II. 360+ Eclipsing Binaries with δ Scuti and γ Doradus Components
Authors: Zhou Ai-Ying 
Published: October 2024

Abstract
A comprehensive analysis of 75,369 stars from Gaia DR3 has led to the serendipitous discovery of 380 eclipsing binaries featuring δ Scuti and γ Doradus pulsators, 45 eclipsing binaries exhibiting rotational variability, and 8 new RR Lyrae stars. Moreover, this study has confirmed 12,145 δ Scuti stars (including 8710 new) and 8192 γ Doradus stars (including 7531 new). These findings substantially expand the existing catalogs of δ Scuti and γ Doradus stars, now encompassing 98,968 and 19,466 stars, respectively, providing a valuable resource for future studies. The remarkable number of newly identified pulsating binaries underscores the significance of this project in validating Gaia variables.
A step forward in botanical exploration with three new Polytrichaceae records from Tibet, China
Authors: Zhao Wei , Wang Zhaoming , Zheng Lina , Naren Gaowa , He Qiang , Han Wei 
Published: October 2024

According to the Species Catalogue of China, Tibet, China, has more than 1,000 species of bryophytes, showing its remarkably high biodiversity. Amongst them, the Polytrichaceae is one of the largest family, with six genera and 25 species, one subspecies and two varieties reported previously.
Based on a field survey and specimen identification, the following species have been newly recorded in the bryoflora of Tibet, namely Oligotrichum obtusatum Broth., Pogonatum contortum (Menzies ex Brid.) Lesq. and Polytrichum sphaerothecium (Besch.) Müll. Hal.
Effectiveness of Cognitive Rehearsal in Addressing Nursing Incivility: An Integrative Review
Authors: Givler Janet L. , Varagona Lynn 
Published: October 2024

Background
Incivility is detrimental to nurses, patients, and health care organizations. Cognitive rehearsal has shown promise in addressing incivility, yet the most recent review of cognitive rehearsal training contained articles published in 2014 and earlier. This review integrates current knowledge of the effectiveness of cognitive rehearsal training in addressing nursing incivility.

Method
Four databases were searched from January 2018 to April 2023. Thematic analysis was used to analyze 22 studies.

Results
Three main themes emerged: (a) theoretical frameworks, (b) participant responses to cognitive rehearsal training, and (c) work culture influences. Nine theoretical frameworks uncover the mechanism behind nursing incivility and provide guidance on how to remedy it.

Conclusion

Cognitive rehearsal training that includes four core components can foster skills and confidence to address nursing incivility and, in turn, decrease its occurrence, but training alone is not sufficient. Nurse managers and leaders need to model civil behavior, support zero tolerance, create a safe environment for reporting incivility, and intervene effectively.

[
J Contin Educ Nurs.
2024;55(11):523–529.]