bluuebunny/crossref_metadata_2025_split huggingface dataset:
Differential gene expression patterns in ST-elevation Myocardial Infarction and Non-ST-elevation Myocardial Infarction
Authors: Elahimanesh Mohammad , Shokri Nafiseh , Mahdinia Elmira , Mohammadi Payam , Parvaz Najmeh , Najafi Mohammad 
Published: February 2024

AbstractThe ST-elevation Myocardial Infarction (STEMI) and Non-ST-elevation Myocardial Infarction (NSTEMI) might occur because of coronary artery stenosis. The gene biomarkers apply to the clinical diagnosis and therapeutic decisions in Myocardial Infarction. The aim of this study was to introduce, enrich and estimate timely the blood gene profiles based on the high-throughput data for the molecular distinction of STEMI and NSTEMI. The text mining data (50 genes) annotated with DisGeNET data (144 genes) were merged with the GEO gene expression data (5 datasets) using R software. Then, the STEMI and NSTEMI networks were primarily created using the STRING server, and improved using the Cytoscape software. The high-score genes were enriched using the KEGG signaling pathways and Gene Ontology (GO). Furthermore, the genes were categorized to determine the NSTEMI and STEMI gene profiles. The time cut-off points were identified statistically by monitoring the gene profiles up to 30 days after Myocardial Infarction (MI). The gene heatmaps were clearly created for the STEMI (high-fold genes 69, low-fold genes 45) and NSTEMI (high-fold genes 68, low-fold genes 36). The STEMI and NSTEMI networks suggested the high-score gene profiles. Furthermore, the gene enrichment suggested the different biological conditions for STEMI and NSTEMI. The time cut-off points for the NSTEMI (4 genes) and STEMI (13 genes) gene profiles were established up to three days after Myocardial Infarction. The study showed the different pathophysiologic conditions for STEMI and NSTEMI. Furthermore, the high-score gene profiles are suggested to measure up to 3 days after MI to distinguish the STEMI and NSTEMI.
Incidence and risk factors of urinary tract infection in hospitalized patients with spinal cord injury in a hospital of China
Authors: Liu Jiawei , Hao Xiaoxia , Shang Xingru , Chi Ruimin , Xu Tao 
Published: February 2024

AbstractUrinary tract infection (UTI) caused by spinal cord injury (SCI) can have significant morbidity. There is currently a lack of relevant data in China. This study explores incidence and risk factors of UTI in hospitalized patients with SCI in China, and will help healthcare professionals to make informed clinical decisions to reduce the incidence of UTI. This retrospective study analyzed the medical records of patients with SCI who were hospitalized at three campuses of a hospital in central China between August 2014 and August 2023. The files of patients with SCI were reviewed for demographics and clinical characteristics. Logistic regression analysis was performed to identify risk factors associated with UTI. A total of 538 patients were included in this study. The incidence of UTI was 49.8%. Sex, hypoproteinemia, urinary incontinence, bladder irrigation, timing of rehabilitation, duration of indwelling urinary catheter were risk factors of UTI. The implementation of specific preventive measures is anticipated to result in a decrease in the occurrence of UTI among individuals with SCI, consequently enhancing their overall quality of life and prognosis.
NF1 mutations as biomarker of response to immune checkpoint blockades for lung adenocarcinoma patients
Authors: Giraud Jean-Stéphane , Jouinot Anne , Pasmant Eric , Tlemsani Camille 
Published: February 2024

AbstractLittle is known about immune checkpoint inhibitors (ICI) response of NF1-mutated lung adenocarcinomas. 341/4,181 (8.2%) TCGA lung adenocarcinomas samples have a somatic NF1 mutation. NF1-mutated tumors have higher TMB (p < 0.0001), higher expression of immune genes (“hot phenotype”) and higher CD8 + T cell (p = 0.03) and macrophage (p = 0.02) infiltrations compared to NF1 wild-type tumors. NF1 mutation status appears as a candidate predictive biomarker for ICI response in lung adenocarcinoma patients.
ISTVP: Independent single transaction verification protocol for light node using fraud proofs without collaborator
Authors: Lee Minghao , Ma Binhao , Han Di , Wang Dejun , Meng Bo 
Published: February 2024

AbstractMost blockchain users run light nodes on mobile devices. Due to limited storage and computation, light nodes cannot perform transaction validation. This shortage makes opportunities for malicious nodes to produce blocks containing invalid transactions, which results in the loss of funds for light nodes. Fraud proofs play a significant role in ensuring transaction security for light nodes. However, existing fraud proof schemes require honest collaborators and the processing of entire blocks. To address these limitations, Independent Single Transaction Verification Protocol for Light node Using Fraud Proofs without Collaborator called ISTVP is proposed that enables light nodes to independently verify transactions and generate fraud proofs without relying on collaborators or processing the entire block. To support ISTVP, SVST is introduced, an efficient block structure for single‐transaction verification. SVST not only efficiently indexes historical transaction outputs to improve verification efficiency, but also significantly reduces the storage requirements for verifying transactions to . Furthermore, the authors analyze the security of ISTVP and demonstrate that it satisfies both persistence and liveness, while maintaining the level of security of full node.
Rethinking the 67 Hz QPO in GRS 1915+105: Type C quasi-periodic oscillations at the innermost stable circular orbit
Authors: Motta S. E. , Belloni T. M. 
Published: February 2024

Context. We study quasi-periodic oscillations (QPO) at low and high frequency in the variability of the high-energy emission from black hole binaries and their physical interpretation in terms of signatures of General Relativity in the strong-field regime.
Aims. We wish to understand the nature of the 67 Hz QPOs observed in the X-ray emission of the peculiar black hole binary GRS 1915+105 within the general classification of QPOs, and to determine the spin of the black hole in the system by applying the relativistic precession model (RPM).
Methods. Within the RPM, the only relativistic frequency that is stable in time over a wide range of accretion rates and can be as low as 67 Hz (for a dynamically measured black hole mass) is the nodal frequency at the innermost stable circular orbit (ISCO). In the application of the model, this corresponds to type C QPOs. Under this assumption, it is possible to measure the spin of the black hole by using the mass of the black hole previously obtained via dynamical measurements. We re-analysed a large number of Rossi-XTE observations to determine whether other timing features confirm this hypothesis.
Results. The identification of the 67 Hz QPO as the nodal frequency at ISCO yields a value of 0.706 ± 0.034 for the black hole spin. With this spin, the only two QPO detections at higher frequencies available in the literature are consistent with being orbital frequencies at a radius outside ISCO. The high-frequency bumps often observed at frequencies between 10 and 200 Hz follow the correlation expected for orbital and periastron-precession frequencies at even larger radii.
Tracking solar radio bursts using Bayesian multilateration
Authors: Cañizares L. A. , Badman S. T. , Maloney S. A. , Owens M. J. , Weigt D. M. , Carley E. P. , Gallagher P. T. 
Published: February 2024

Context. Solar radio bursts (SRBs), such as Type IIs and IIIs, are emitted by electrons propagating through the corona and interplanetary space. Tracking such bursts is key to understanding the properties of accelerated electrons and radio wave propagation as well as the local plasma environment that they propagate through.
Aims. In this work, we present a novel multilateration algorithm called BayEsian LocaLisation Algorithm (BELLA) and validate the algorithm using simulated and observed SRBs. In addition, apparent SRB positions from BELLA are compared with comparable localisation methods and the predictions of solar wind models.
Methods. BELLA uses Bayesian inference to create probabilistic distributions of source positions and their uncertainties. This facilitates the estimation of algorithmic, instrumental, and physical uncertainties in a quantitative manner.
Results. We validated BELLA using simulations and a Type III SRB observed by STEREO A and STEREO B at ±116° from the Sun-Earth line and by Wind at L1. BELLA tracked the Type III source from ∼10–150 R⊙ (2–0.15 MHz) along a spiral trajectory. This allowed for an estimate of an apparent solar wind speed of vsw ∼ 400 km s−1 and a source longitude of ϕ0 ∼ 30°. We compared these results with well-established methods of positioning: Goniopolarimetric (GP), analytical time-difference-of-arrival (TDOA), and Solar radio burst Electron Motion Tracker (SEMP). We found them to be in agreement with the results obtained by BELLA. Additionally, the results aligned with solar wind properties assimilated by the Heliospheric Upwind Extrapolation with time dependence (HUXt) model.
Conclusions. We have validated BELLA and used it to identify apparent source positions as well as velocities and densities of the solar wind. Furthermore, we identified higher than expected electron densities, suggesting that the true emission sources were at lower altitudes than those identified by BELLA, an effect that may be due to appreciable scattering of electromagnetic waves by electrons in interplanetary space.
Magnetochronology of solar-type star dynamos
Authors: Noraz Q. , Brun A. S. , Strugarek A. 
Published: February 2024

Aims. In this study, we analyse the magnetic field properties of a set of 15 global magnetohydrodynamic (MHD) simulations of solar-type star dynamos conducted using the ASH code. Our objective is to enhance our understanding of these properties by comparing theoretical results to current observations, and to finally provide fresh insights into the field.
Methods. We analysed the rotational and magnetic properties as a function of various stellar parameters (mass, age, and rotation rate) in a ‘Sun in time’ approach in our extended set of 3D MHD simulations. To facilitate direct comparisons with stellar magnetism observations using various Zeeman-effect techniques, we decomposed the numerical data into vectorial spherical harmonics.
Results.A comparison of the trends we find in our simulations set reveals a promising overall agreement with the observational context of stellar magnetism, enabling us to suggest a plausible scenario for the magneto-rotational evolution of solar-type stars. In particular, we find that the magnetic field may reach a minimum amplitude at a transition value of the Rossby number near unity. This may have important consequences on the long-term evolution of solar-type stars, by impacting the relation between stellar age, rotation, and magnetism. This supports the need for future observational campaigns, especially for stars in the high Rossby number regime.
Dissipationless collapse and the dynamical mass–ellipticity relation of elliptical galaxies in Newtonian gravity and MOND
Authors: Di Cintio Pierfrancesco 
Published: February 2024

Context. Recent observational studies proposed an empirical relation between the dark-to-total mass ratio and ellipticity in elliptical galaxies based on their observed total dynamical mass-to-light ratio data M/L = (14.1 ± 5.4)ϵ. In other words, the larger the content of dark matter in the galaxy, the more the stellar component will be flattened. If true, this observation appears to be in stark contrast with the commonly accepted galaxy formation scenario, whereby this process takes place inside dark halos with reasonably spherical symmetry.
Aims. Comparing the processes of dissipationless galaxy formation in different theories of gravity and the emergence of the galaxy scaling relations therein provides an important framework within which, in principle, one can discriminate between these processes.
Methods. By means of collisionless N-body simulations in modified Newtonian dynamics (MOND) and Newtonian gravity with and without active dark matter halos, with both spherical and clumpy initial structure, I study the trends of intrinsic and projected ellipticities, Sérsic index, and anisotropy with the total dynamical-to-stellar mass ratio.
Results. I show that the end products of both cold spherical collapses and mergers of smaller clumps show an increasing departure from spherical symmetry for increasing values of the total dynamical-to-stellar mass ratio, at least in a range of halo masses. The equivalent Newtonian systems of the end products of MOND collapses show a similar behaviour. However, the M/L relation obtained from the numerical experiments in both gravities is rather different from that reported by Deur and coauthors.
Searching for X-ray counterparts of unassociated Fermi-LAT sources and rotation-powered pulsars with SRG/eROSITA
Authors: Mayer Martin G. F. , Becker Werner 
Published: February 2024

Context. The latest source catalog of the Fermi-LAT telescope contains more than 7000 γ-ray sources at giga-electronvolt energies, with the two dominant source classes thought to be blazars and rotation-powered pulsars. Despite continuous follow-up efforts, around 2600 sources have no known multiwavelength association.
Aims. Our target is the identification of possible (young and recycled) pulsar candidates in the sample of unassociated γ-ray sources via their characteristic X-ray and γ-ray emission. To achieve this, we cross-matched the Fermi-LAT catalog with the catalog of X-ray sources in the western Galactic hemisphere from the first four all-sky surveys of eROSITA on the Spektrum-Roentgen-Gamma (SRG) mission. We complement this by identifying X-ray counterparts of known pulsars detected at γ-ray and radio energies in the eROSITA data.
Methods. We used a Bayesian cross-matching scheme to construct a probabilistic catalog of possible pulsar-type X-ray counterparts to Fermi-LAT sources. Our method combines the overlap of X-ray and γ-ray source positions with a probabilistic classification (into pulsar and blazar candidates) of each source based on its γ-ray properties and a prediction on the X-ray flux of pulsar- or blazar-type counterparts. Finally, an optical and infrared counterpart search was performed to exclude coronally emitting stars and active galactic nuclei from our catalog.
Results. We provide a catalog of our prior γ-ray-based classifications of all 2600 unassociated sources in the Fermi-LAT catalog, with around equal numbers of pulsar and blazar candidates. Our final list of candidate X-ray counterparts to suspected new high-energy pulsars, cleaned for spurious detections and sources with obvious non-pulsar counterparts, contains around 900 X-ray sources, the vast majority of which lie in the 95% γ-ray error ellipse. We predict between 30 and 40 new pulsars among our top 200 candidates, with around equal numbers of young and recycled pulsars. This candidate list may serve as input to future follow-up campaigns, looking directly for pulsations or for the orbital modulation of possible binary companions, where it may allow for a drastic reduction in the number of candidate locations to search. We furthermore detect the X-ray counterparts of 15 known rotation-powered pulsars, which were not seen in X-rays before.
Experimental investigations of diacetylene ice photochemistry in Titan’s atmospheric conditions
Authors: Fleury Benjamin , Gudipati Murthy S. , Couturier-Tamburelli Isabelle 
Published: February 2024

Context. A large fraction of the organic species produced photochemically in the atmosphere of Titan can condense to form ice particles in the stratosphere and in the troposphere. According to various studies, diacetylene (C4H2) condenses below 100 km where it can be exposed to ultraviolet radiation.
Aims. We studied experimentally the photochemistry of diacetylene ice (C4H2) to evaluate its potential role in the lower altitude photochemistry of Titan’s atmospheric ices.
Methods. C4H2 ice films were irradiated with near-ultraviolet (near-UV) photons (λ > 300 nm) with different UV sources to assess the impact of the wavelengths of photons on the photochemistry of C4H2. The evolution of the ice’s composition was monitored using spectroscopic techniques.
Results. Our results reveal that diacetylene ice is reactive through singlet-triplet absorption, similar to the photochemistry of other organic ices of Titan (such as dicyanoacetylene C4N2 ice) that we investigated previously. Several chemical processes occurred during the photolysis: the hydrogenation of C4H2 to form other C4 hydrocarbons (vinylacetylene C4H4 to butane C4H10); the formation of larger and highly polymerizable hydrocarbons, such as triacetylene (C6H2); and the formation of an organic polymer that is stable at room temperature.
Conclusions. The nondetection of diacetylene ice in Titan’s atmosphere or surface could be rationalized based on our experimental results that C4H2 is photochemically highly reactive in the solid phase when exposed to near-UV radiation that reaches Titan’s lower altitudes and surface. C4H2 may be one of the key molecules promoting the chemistry in the ices and aerosols of Titan’s haze layers, especially in the case of co-condensation with other organic volatiles, with which it could initiate more complex solid-phase chemistry.
Constraints on the evolution of the Triton atmosphere from occultations: 1989–2022
Authors: Sicardy B. , Tej A. , Gomes-Júnior A. R. , Romanov F. D. , Bertrand T. , Ashok N. M. , Lellouch E. , Morgado B. E. , Assafin M. , Desmars J. , Camargo J. I. B. , Kilic Y. , Ortiz J. L. , Vieira-Martins R. , Braga-Ribas F. , Ninan J. P. , Bhatt B. C. , Pramod Kumar S. , Swain V. , Sharma S. , Saha A. , Ojha D. K. , Pawar G. , Deshmukh S. , Deshpande A. , Ganesh S. , Jain J. K. , Mathew S. K. , Kumar H. , Bhalerao V. , Anupama G. C. , Barway S. , Brandeker A. , Florén H. G. , Olofsson G. , Bruno G. , Mao Y. M. , Ye R. H. , Zou Q. Y. , Sun Y. K. , Shen Y. Y. , Zhao J. Y. , Grishin D. N. , Romanova L. V. , Marchis F. , Fukui K. , Kukita R. , Benedetti-Rossi G. , Santos-Sanz P. , Dhyani N. , Gokhale A. , Kate A. 
Published: February 2024

Context. In about 2000, the south pole of Triton experienced an extreme summer solstice that occurs every ∼650 years, when the subsolar latitude reached about 50°S. Bracketing this epoch, a few occultations probed the Triton atmosphere in 1989, 1995, 1997, 2008, and 2017. A recent ground-based stellar occultation observed on 6 October 2022 provides a new measurement of the atmospheric pressure on Triton. This is presented here.
Aims. The goal is to constrain the volatile transport models (VTMs) of the Triton atmosphere. The atmosphere is basically in vapor pressure equilibrium with the nitrogen ice at its surface.
Methods. Fits to the occultation light curves yield the atmospheric pressure of Triton at the reference radius 1400 km, from which the surface pressure is deduced.
Results. The fits provide a pressure p1400 = 1.211 ± 0.039 μbar at radius 1400 km (47 km altitude), from which a surface pressure of psurf = 14.54 ± 0.47 μbar is deduced (1σ error bars). To within the error bars, this is identical to the pressure derived from the previous occultation of 5 October 2017, p1400 = 1.18 ± 0.03 μbar and psurf = 14.1 ± 0.4 μbar, respectively. Based on recent models of the volatile cycles of Triton, the overall evolution of the surface pressure over the last 30 years is consistent with N2 condensation taking place in the northern hemisphere. However, models typically predict a steady decrease in the surface pressure for the period 2005-2060, which is not confirmed by this observation. Complex surface-atmosphere interactions, such as ice albedo runaway and formation of local N2 frosts in the equatorial regions of Triton, could explain the relatively constant pressure between 2017 and 2022.
Measuring Hearing Aid Satisfaction in Everyday Listening Situations: Retrospective and In Situ Assessments Complement Each Other
Authors: Lelic Dina , Wolters Florian , Schinkel-Bielefeld Nadja 
Published: February 2024

Abstract
Background Recently, we developed a hearing-related lifestyle questionnaire (HEARLI-Q), which asks respondents to rate their hearing aid (HA) satisfaction in 23 everyday listening situations. It is unknown how HA satisfaction on the retrospective HEARLI-Q scale compares with HA satisfaction measured on the same scale implemented in Ecological Momentary Assessment (EMA).
Purpose To learn how retrospective (HEARLI-Q) and in situ (EMA) assessments can complement each other.
Research Design An observational study.
Study Sample Twenty-one experienced HA users.
Data Collection and Analysis The participants first filled out the HEARLI-Q questionnaire, followed by a 1-week EMA trial using their own HAs. HA satisfaction ratings were compared between the two questionnaires and the underlying drivers of discrepancies in HA satisfaction ratings were evaluated.
Results HA satisfaction ratings were significantly higher in EMA for speech communication with one or several people. Hearing difficulty in these situations was rated higher in HEARLI-Q than in EMA, but occurrence of those difficult listening situations was also rated to be lower. When comparing only the situations that occur on daily or weekly basis, the two questionnaires had similar HA satisfaction ratings.
Conclusions Lower occurrence of difficult listening situations seems to be the key driver of discrepancies in HA satisfaction ratings between EMA and HEARLI-Q. The advantage of EMA is that it provides insight into an individual's day-to-day life and is not prone to memory bias. HEARLI-Q, on the other hand, can capture situations that occur infrequently or are inconvenient to report in the moment. Administering HEARLI-Q and EMA in combination could give a more holistic view of HA satisfaction.
Comparison of Different Surgical Approaches for Treating Aortic Graft Infections
Authors: Xia Yu , Sun Lizhong , Jian Kaitao , Peng Hao , Lin Yi , Liu Wei 
Published: February 2024

Abstract
Background There is still no guideline or consensus on the treatment of aortic graft infection. This study reported and compared conservative and surgical treatment and different surgical methods for aortic graft infection.
Methods Data from aortic graft infections treated at our institution between February 2017 and June 2022 were retrospectively analyzed. Clinical data and surgical approaches were evaluated.
Results This article retrospectively analyzed the treatment and prognosis of 48 patients (43 males) with aortic graft infection. The patients were divided into conservative treatment group (n = 15) and surgical treatment group (n = 33). During follow-up, the mortality rate of the conservative treatment group was significantly higher than that of the surgical treatment group (p < 0.05). The survival curve also showed that the survival time of the surgical treatment group was longer than that of the conservative treatment group (p < 0.05). The surgical treatment group included local treatment (n = 5), in situ replacement (n = 8), and bypass surgery (n = 20) groups. There was no significant difference in the mortality rate at 1 month or final follow-up among the local treatment, in situ replacement, and bypass surgery groups.
Conclusion Surgical treatment is the optimal option for treating aortic graft infections compared to conservative treatment.