bluuebunny/crossref_metadata_2025_split huggingface dataset:
Portal Vein Stenosis Following Neoadjuvant Therapy With MRgART and Surgery for Pancreatic Cancer: A Case Report
Authors: Adler Evan , Keit Emily , Al-Roubaie Mustafa , Kis Bela , Drake Justin A. , Denbo Jason W. , Hodul Pam J. , Hoffe Sarah E. , Frakes Jessica M. , Palm Russell F. 
Published: August 2024

Abstract
Portal vein stenosis (PVS) is a rare but potentially devastating complication arising after definitive treatment of pancreatic cancer. The condition can manifest as symptomatic ascites, abdominal pain, splenomegaly, thrombocytopenia, as well as hemorrhage secondary to gastric or esophageal varices. The etiology is often multifactorial but has been associated with tumor progression, chemotherapy, vascular surgery, and radiation. We present a case in which a man with borderline-resectable pancreatic cancer developed symptomatic ascites secondary to PVS following treatment with neoadjuvant chemotherapy and subsequent 5-fraction MRI-guided adaptive radiation therapy and pancreaticoduodenectomy with vascular reconstruction. Though the incidence of PVS after ablative radiation therapy and surgery for pancreatic cancer appears to be low, it may be under-reported, and patients should be closely monitored in the setting of re-irradiation or planned vascular reconstruction. These findings may help inform future radiation therapy treatment planning guidelines to avoid excessive dose to the portal vein.
Revising Properties of Planet–Host Binary Systems. IV. The Radius Distribution of Small Planets in Binary Star Systems Is Dependent on Stellar Separation*
Authors: Sullivan Kendall , Kraus Adam L. , Berger Travis A. , Dupuy Trent J. , Evans Elise , Gaidos Eric , Huber Daniel , Ireland Michael J. , Mann Andrew W. , Petigura Erik A. , Thao Pa Chia , Wood Mackenna L. , Zhang Jingwen 
Published: August 2024

Abstract
Small planets (R

p
≤ 4 R
⊕) are divided into rocky super-Earths and gaseous sub-Neptunes separated by a radius gap, but the mechanisms that produce these distinct planet populations remain unclear. Binary stars are the only main-sequence systems with an observable record of the protoplanetary disk lifetime and mass reservoir, and the demographics of planets in binaries may provide insights into planet formation and evolution. To investigate the radius distribution of planets in binary star systems, we observed 207 binary systems hosting 283 confirmed and candidate transiting planets detected by the Kepler mission, then recharacterized the planets while accounting for the observational biases introduced by the secondary star. We found that the population of planets in close binaries (ρ ≤ 100 au) is significantly different from the planet population in wider binaries (ρ > 300 au) or single stars. In contrast to planets around single stars, planets in close binaries appear to have a unimodal radius distribution with a peak near the expected super-Earth peak of R

p
∼ 1.3 R
⊕ and a suppressed population of sub-Neptunes. We conclude that we are observing the direct impact of a reduced disk lifetime, smaller mass reservoir, and possible altered distribution of solids reducing the sub-Neptune formation efficiency. Our results demonstrate the power of binary stars as a laboratory for exploring planet formation and as a controlled experiment of the impact of varied initial conditions on mature planet populations.
The First Evidence of a Host Star Metallicity Cutoff in the Formation of Super-Earth Planets
Authors: Boley Kiersten M. , Christiansen Jessie L. , Zink Jon , Hardegree-Ullman Kevin , Lee Eve J. , Hopkins Philip F. , Wang 王 Ji 吉 , Fernandes Rachel B. , Bergsten Galen J. , Bhure Sakhee 
Published: August 2024

Abstract
Planet formation is expected to be severely limited in disks of low metallicity, owing to both the small solid mass reservoir and the low-opacity accelerating the disk gas dissipation. While previous studies have found a weak correlation between the occurrence rates of small planets (≲4R
⊕) and stellar metallicity, so far no studies have probed below the metallicity limit beyond which planet formation is predicted to be suppressed. Here, we constructed a large catalog of ∼110,000 metal-poor stars observed by the TESS mission with spectroscopically derived metallicities, and systematically probed planet formation within the metal-poor regime ([Fe/H] ≤−0.5) for the first time. Extrapolating known higher-metallicity trends for small, short-period planets predicts the discovery of ∼68 super-Earths around these stars (∼85,000 stars) after accounting for survey completeness; however, we detect none. As a result, we have placed the most stringent upper limit on super-Earth occurrence rates around metal-poor stars (−0.75 < [Fe/H] ≤ −0.5) to date, ≤ 1.67%, a statistically significant (p-value = 0.000685) deviation from the prediction of metallicity trends derived with Kepler and K2. We find a clear host star metallicity cliff for super-Earths that could indicate the threshold below which planets are unable to grow beyond an Earth-mass at short orbital periods. This finding provides a crucial input to planet-formation theories, and has implications for the small planet inventory of the Galaxy and the galactic epoch at which the formation of small planets started.
The Massive and Distant Clusters of WISE Survey 2: A Stacking Analysis Investigating the Evolution of Star Formation Rates and Stellar Masses in Groups and Clusters
Authors: Trudeau A. , Gonzalez Anthony H. , Thongkham K. , Lee Kyoung-Soo , Alberts Stacey , Brodwin M. , Connor Thomas , Eisenhardt Peter R. M. , Moravec Emily , Puvvada Eshwar , Stanford S. A. 
Published: August 2024

Abstract
The evolution of galaxies depends on their masses and local environments; understanding when and how environmental quenching starts to operate remains a challenge. Furthermore, studies of the high-redshift regime have been limited to massive cluster members, owing to sensitivity limits or small fields of view when the sensitivity is sufficient, intrinsically biasing the picture of cluster evolution. In this work, we use stacking to investigate the average star formation history of more than 10,000 groups and clusters drawn from the Massive and Distant Clusters of WISE Survey 2. Our analysis covers near-ultraviolet to far-infrared wavelengths, for galaxy overdensities at 0.5 ≲ z ≲ 2.54. We employ spectral energy distribution fitting to measure the specific star formation rates (sSFRs) in four annular apertures with radii between 0 and 1000 kpc. At z ≳ 1.6, the average sSFR evolves similarly to the field in both the core and the cluster outskirts. Between

z

¯

=
1.60

and

z

¯

=
1.35

, the sSFR in the core drops sharply, and it continues to fall relative to the field sSFR at lower redshifts. We interpret this change as evidence that the impact of environmental quenching dramatically increases at z ∼ 1.5, with the short time span of the transition suggesting that the environmental quenching mechanism dominant at this redshift operates on a rapid timescale. We find indications that the sSFR may decrease with increasing host halo mass, but lower-scatter mass tracers than the signal-to-noise ratio are needed to confirm this relationship.
The Complex Star Formation History of the Halo of NGC 5128 (Cen A)
Authors: Aghdam Sima T. , Javadi Atefeh , Hashemi Seyedazim , Abdollahi Mahdi , van Loon Jacco Th. , Khosroshahi Habib , Golshan Roya H. , Saremi Elham , Saberi Maryam 
Published: August 2024

Abstract
NGC 5128 (Cen A) is the nearest giant elliptical galaxy and one of the brightest extragalactic radio sources in the sky, boasting a prominent dust lane and jets emanating from its nuclear supermassive black hole. In this paper, we construct the star formation history (SFH) of two small fields in the halo of NGC 5128: a northeastern field (Field 1) at a projected distance of ∼18.8 kpc from the center, and a southern field (Field 2) ∼9.9 kpc from the center. Our method is based on identifying long-period variable (LPV) stars that trace their sibling stellar population and hence historical star formation due to their high luminosity and strong variability; we identified 395 LPV stars in Field 1 and 671 LPV stars in Field 2. Even though the two fields are ∼28 kpc apart on opposite sides from the center, they show similar SFHs. In Field 1, the star formation rate (SFR) increased significantly around t ∼ 800 Myr and t ∼ 3.8 Gyr and in Field 2, the SFR increased considerably around t ∼ 800 Myr, t ∼ 3.8 Gyr, and t ∼ 6.3 Gyr, where t is the lookback time. The increase in SFR ∼800 Myr ago agrees with previous suggestions that the galaxy experienced a merger around that time. The SFH reconstructed from LPV stars supports a scenario in which multiple episodes of nuclear activity lead to episodic jet-induced star formation. While there is no catalog of LPV stars for the central part of NGC 5128, applying our method to the outer regions (for the first time in a galaxy outside the Local Group) has enabled us to put constraints on the complex evolution of this cornerstone galaxy.
Deeper, Sharper, Faster: Application of Efficient Transformer to Galaxy Image Restoration
Authors: Park Hyosun , Jo Yongsik , Kang Seokun , Kim Taehwan , Jee M. James 
Published: August 2024

Abstract
The Transformer architecture has revolutionized the field of deep learning over the past several years in diverse areas, including natural language processing, code generation, image recognition, and time-series forecasting. We propose to apply Zamir et al.'s efficient transformer to perform deconvolution and denoising to enhance astronomical images. We conducted experiments using pairs of high-quality images and their degraded versions, and our deep learning model demonstrates exceptional restoration of photometric, structural, and morphological information. When compared with the ground-truth James Webb Space Telescope images, the enhanced versions of our Hubble Space Telescope–quality images reduce the scatter of isophotal photometry, Sérsic index, and half-light radius by factors of 4.4, 3.6, and 4.7, respectively, with Pearson correlation coefficients approaching unity. The performance is observed to degrade when input images exhibit correlated noise, point-like sources, and artifacts. We anticipate that this deep learning model will prove valuable for a number of scientific applications, including precision photometry, morphological analysis, and shear calibration.
Cold Filaments Formed in Hot Wake Flows Uplifted by Active Galactic Nucleus Bubbles in Galaxy Clusters
Authors: Duan Xiaodong , Guo Fulai 
Published: August 2024

Abstract
Multiwavelength observations indicate that the intracluster medium in some galaxy clusters contains cold filaments, while their formation mechanism remains debated. Using hydrodynamic simulations, we show that cold filaments could naturally condense out of the hot gaseous wake flows uplifted by jet-inflated active galactic nucleus (AGN) bubbles. Consistent with observations, the simulated filaments extend to tens of kiloparsecs from the cluster center, with a representative mass of 108–109
M
⊙ for a typical AGN outburst energy of 1060 erg. They show smooth velocity gradients, stretching typically from inner inflows to outer outflows with velocity dispersions of several hundred kilometers per second. The properties of cold filaments are affected substantially by the jet properties. Compared to kinetic-energy-dominated jets, it is easier for thermal-energy-dominated jets to produce long cold filaments with large masses, as observed. AGN jets with an early turn-on time, a low jet base, or a very high power tend to overheat the cluster center and produce short cold filaments that take a relatively long time to condense out.
The Differences in the Origination and Properties of the Near-Earth Solar Wind between Solar Cycles 23 and 24
Authors: Shi Xinzheng , Fu Hui , Huang Zhenghua , Yan Limei , Ma Chi , Huangfu Chenxi , Song Hongqiang , Xia Lidong 
Published: August 2024

Abstract
The dependence of the sources and properties of the near-Earth solar wind on solar cycle activity is an important issue in solar and space physics. We use the improved “two-step” mapping procedure that takes into account the initial acceleration processes to trace the near-Earth solar winds back to their source regions from 1999–2020, covering solar cycles (SCs) 23 and 24. Then, the solar wind is categorized into coronal hole (CH), active region (AR), and quiet Sun (QS) solar wind based on the source region type. We find that the proportions of CH and AR (QS) wind during SC 23 are higher (lower) than those during SC 24. During solar maximum and declining phases, the magnetic field strength, speed, helium abundance (A
He), and charge states of all three types of solar wind during SC 23 are generally higher than those during SC 24. During solar minimum, these parameters of solar wind are generally lower during SC 23 than those during SC 24. There is a significant decrease in the charge states of all three types of solar wind during the solar minimum of SC 23. The present statistical results demonstrate that the sources and properties of the solar wind are both influenced by solar cycle amplitude. The temperatures of AR, QS, and CH regions exhibit significant differences at low altitudes, whereas they are almost uniform at high altitudes.
The Instability Mechanism of Compact Multiplanet Systems
Authors: Lammers Caleb , Hadden Sam , Murray Norman 
Published: August 2024

Abstract
To improve our understanding of orbital instabilities in compact planetary systems, we compare suites of N-body simulations against numerical integrations of simplified dynamical models. We show that, surprisingly, dynamical models that account for small sets of resonant interactions between the planets can accurately recover N-body instability times. This points toward a simple physical picture in which a handful of three-body resonances, generated by interactions between nearby two-body mean motion resonances, overlap and drive chaotic diffusion, leading to instability. Motivated by this, we show that instability times are well described by a power law relating instability time to planet separations, measured in units of fractional semimajor axis difference divided by the planet-to-star mass ratio to the 1/4 power, rather than the frequently adopted 1/3 power implied by measuring separations in units of mutual Hill radii. For idealized systems, the parameters of this power-law relationship depend only on the ratio of the planets’ orbital eccentricities to the orbit-crossing value, and we report an empirical fit to enable quick instability time predictions. This relationship predicts that observed systems comprised of three or more sub-Neptune-mass planets must be spaced with period ratios

P

≳

1.35

and that tightly spaced systems (

P

≲

1.5

) must possess very low eccentricities (e ≲ 0.05) to be stable for more than 109 orbits.
Al2O Photochemistry
Authors: Trabelsi Tarek , Francisco Joseph S. 
Published: August 2024

Abstract
The chemistry within the interstellar medium (ISM) is notably influenced by the interplay between kinetics and photochemical processes, which play significant roles in both the formation and destruction of molecular species. This study focuses on theoretical investigations of Al2O photochemistry, aiming to elucidate the mechanisms underlying the production of AlO and Al in the VY-CMa star. Utilizing advanced theoretical methodologies, we explore the lowest electronic states with singlet and triplet spin multiplicities in linear Al2O. We investigated the photostability of Al2O in the near UV‒Vis region, revealing the low likelihood of photodissociation and photoconversion while suggesting the plausibility of fluorescence and phosphorescence phenomena. Calculations also identify three prominent peaks in the UV range at 261.5, 206.2, and 199 nm. Finally, Al2O is predicted to be photostable and cannot be the parent molecule of the diatomic AlO or even the astrochemical reservoir of atomic aluminum. These results contribute to improving the astronomical models in simulating aluminum chemistry in the ISM.
Do All the Quasars and High-excitation Radio Galaxies (HERGs) in the 3CRR Catalog Contain a Magnetically Arrested Disk (MAD)?
Authors: Li Shuang-Liang , Zuo Wenwen , Cao Xinwu 
Published: August 2024

Abstract
Based on the magnetization, an accretion disk with a large-scale magnetic field can be separated into either standard and normal evolution or magnetically arrested disk (MAD), which are difficult to identify from observations. It is still unclear whether all the radio-loud active galactic nuclei (RLAGNs) with a thin disk and strong radio emissions contain a MAD. We investigate this issue by utilizing the 3CRR catalog. We compile a sample of 35 quasars and 14 high-excitation radio galaxies powered by a thin accretion disk. In order to consistently compare with the MAD sample given by Li et al., the optical-UV emissions of our sample are all detected by the Hubble Space Telescope. It is found that the average X-ray luminosity (L
X) of our sample is about 5.0 times higher than that of radio-quiet active galactic nuclei with matching optical-UV luminosity (L
UV), in general accord with the factor of 4.5 times in MAD sample within the uncertainty. The relationship between radio (5 GHz) and X-ray (2 keV) luminosities in the 3CRR sources is also found to be consistent with the MAD sample. Furthermore, the jet efficiencies of 3CRR sources are consistent with those from the GRMHD simulations of MAD. Therefore, we suggest that probably all the quasars and at least a fraction of high-excitation radio galaxies in the 3CRR catalog, and perhaps all the RLAGNs with strong radio emissions contain a MAD.
Cyclical Period Changes in Cataclysmic Variables: A Statistical Study
Authors: Souza Leandro , Baptista Raymundo 
Published: August 2024

Abstract
We report the results of a statistical study of cyclical period changes in cataclysmic variables (CVs). Assuming the third-body hypothesis as the cause of period changes, we estimate the third-body mass, m
3, and its separation from the binary, a
3, for 21 CVs showing cyclical period changes from well-sampled observed-minus-calculated diagrams covering more than a decade of observations. The inferred a
3 values are independent of the binary orbital period, P
orb, whereas the m
3 values increase with P
orb by 1 order of magnitude from the shortest period (oldest) to the longest period (youngest) systems, implying significant mass loss from the third body with time. A model for the time evolution of the triple system is not able to simultaneously explain the observed behavior of the m
3(P
orb) and a
3(P
orb) distributions because the combined mass loss from the binary and the third body demands an increase in orbital separation by factors ∼140 as the binary evolves toward shorter P
orb's, in clear disagreement with the observed distribution. We conclude that the third-body hypothesis is statistically inconsistent and cannot be used to explain cyclical period changes observed in CVs. On the other hand, the diagram of the amplitude of the period change versus the CV donor-star mass is consistent both with the alternative hypothesis that the observed cyclical period changes are a consequence of magnetic activity in the solar-type donor star, and with the standard evolutionary scenario for CVs.
Extended Cyclotron Resonant Heating of the Turbulent Solar Wind
Authors: Bowen Trevor A. , Vasko Ivan Y. , Bale Stuart D. , Chandran Benjamin D. G. , Chasapis Alexandros , Dudok de Wit Thierry , Mallet Alfred , McManus Michael , Meyrand Romain , Pulupa Marc , Squire Jonathan 
Published: August 2024

Abstract
Circularly polarized, nearly parallel propagating waves are prevalent in the solar wind at ion-kinetic scales. At these scales, the spectrum of turbulent fluctuations in the solar wind steepens, often called the transition range, before flattening at sub-ion scales. Circularly polarized waves have been proposed as a mechanism to couple electromagnetic fluctuations to ion gyromotion, enabling ion-scale dissipation that results in observed ion-scale steepening. Here we study Parker Solar Probe observations of an extended stream of fast solar wind ranging from ∼15 to 55 R
⊙. We demonstrate that, throughout the stream, transition range steepening at ion scales is associated with the presence of significant left-handed ion-kinetic-scale waves, which are thought to be ion cyclotron waves. We implement quasilinear theory to compute the rate at which ions are heated via cyclotron resonance with the observed circularly polarized waves given the empirically measured proton velocity distribution functions. We apply the Von Kármán decay law to estimate the turbulent decay of the large-scale fluctuations, which is equal to the turbulent energy cascade rate. We find that the ion cyclotron heating rates are correlated with, and amount to a significant fraction of, the turbulent energy cascade rate, implying that cyclotron heating is an important dissipation mechanism in the solar wind.
An Earth Encounter as the Cause of Chaotic Dynamics in Binary Asteroid (35107) 1991VH
Authors: Meyer Alex J. , Fuentes-Muñoz Oscar , Gkolias Ioannis , Tsiganis Kleomenis , Pravec Petr , Naidu Shantanu , Scheeres Daniel J. 
Published: August 2024

Abstract
Among binary asteroids, (35107) 1991VH stands out as unique given the likely chaotic rotation within its secondary component. The source of this excited dynamical state is unknown. In this work, we demonstrate that a past close encounter with Earth could have provided the necessary perturbation to allow the natural internal dynamics, characterized by spin–orbit coupling, to evolve the system into its current dynamical state. In this hypothesis, the secondary of 1991VH was previously in a classical 1:1 spin–orbit resonance with an orbit period likely between 28 and 35 hr before being perturbed by an Earth encounter within ∼80,000 km. We find that if the energy dissipation within the secondary is relatively inefficient, this excited dynamical state could persist to today and produce the observed ground-based measurements. Coupled with the orbital history of 1991VH, we can then place a constraint on the tidal dissipation parameters of the secondary.
Improving Prelicensure Student Learning and Experience With Interactive Online Learning Modules
Authors: Stuffle Megan E. 
Published: August 2024

Background:

Fundamentals of Nursing students at a large school of nursing in the Midwest reported difficulty using their course textbooks. There was also an increase in course failures and a decrease in performance on a Fundamentals of Nursing National Council Licensure Examination (NCLEX-RN
®
) preparatory proctored examination.

Method:
A pilot project was implemented to evaluate the effectiveness of interactive, online learning modules compared to textbook readings on student performance, access and use of resources, and student experience.

Results:
Following the pilot there was a significant improvement in course grades among traditional but not accelerated students using the modules compared to those using the textbook. Students reported that the modules were more engaging, cost-effective, and appealing to various learning styles. Weaknesses identified were the module lengths and technological concerns.

Conclusion:

The online, interactive modules engaged students with course materials, reduced costs, and may have changed student performance. Additional research is needed among students in other courses and programs.

[
J Nurs Educ
. 2024;63(X):XXX–XXX.]