bluuebunny/crossref_metadata_2025_split huggingface dataset:
Return to work in young and middle-aged colorectal cancer survivors: Factors influencing self-efficacy, fear, resilience, and financial toxicity
Authors: Hu Dan , Li Yue , Zhang Hua , Wang Lian-Lian , Liu Wen-Wen , Yang Xin , Xiao Ming-Zhao , Zhang Hao-Ling , Li Juan 
Published: December 2024

BACKGROUND
Return to work (RTW) serves as an indication for young and middle-aged colorectal cancer (CRC) survivors to resume their normal social lives. However, these survivors encounter significant challenges during their RTW process. Hence, scientific research is necessary to explore the barriers and facilitating factors of returning to work for young and middle-aged CRC survivors.
AIM
To examine the current RTW status among young and middle-aged CRC survivors and to analyze the impact of RTW self-efficacy (RTW-SE), fear of progression (FoP), eHealth literacy (eHL), family resilience (FR), and financial toxicity (FT) on their RTW outcomes.
METHODS
A cross-sectional investigation was adopted in this study. From September 2022 to February 2023, a total of 209 participants were recruited through a convenience sampling method from the gastrointestinal surgery department of a class A tertiary hospital in Chongqing. The investigation utilized a general information questionnaire alongside scales assessing RTW-SE, FoP, eHL, FR, and FT. To analyze the factors that influence RTW outcomes among young and middle-aged CRC survivors, Cox regression modeling and Kaplan-Meier survival analysis were used.
RESULTS
A total of 43.54% of the participants successfully returned to work, with an average RTW time of 100 days. Cox regression univariate analysis revealed that RTW-SE, FoP, eHL, FR, and FT were significantly different between the non-RTW and RTW groups (P < 0.05). Furthermore, Cox regression multivariate analysis identified per capita family monthly income, job type, RTW-SE, and FR as independent influencing factors for RTW (P < 0.05).
CONCLUSION
The RTW rate requires further improvement. Elevated levels of RTW-SE and FR were found to significantly increase RTW among young and middle-aged CRC survivors. Health professionals should focus on modifiable factors, such as RTW-SE and FR, to design targeted RTW support programs, thereby facilitating their timely reintegration into mainstream society.
Analisis Pasang Surut di Teluk Davao Filipina Menggunakan Metode Least Square Periode Oktober 2022
Authors: Akbar Agya Muhammad , Pranowo Widodo Setiyo , Bimantara Agung 
Published: December 2024

Teluk Davao yang berada di wilayah yurisdiksi negara Filipina, secara geografis lokasinya berada dekat dengan pulau-pulau terluar di utara Indonesia. Dimana pulau-pulau terluar ini tidak memiliki stasiun pasang surut, sehingga Teluk Davao dianggap dapat merepresentasikan fenomena pasang surut pada pulau-pulau tersebut. Tujuan penelitian ini adalah untuk mengetahui tipe pasang surut pada lokasi penelitian serta mengolah konstanta harmonik pasang surut dengan metode Least Square menggunakan perangkat lunak t_tide yang berbasiskan bahasa pemrograman MatLab. Dari hasil penelitian ini dihasilkan konstanta harmonik sebanyak 32 konstanta yang menghasilkan nilai frekuensi, amplitudo, fase, dan SNR yang selanjutnya dijadikan bahan analisa. Dimana dari 32 konstanta yang didapatkan, 12 konstanta merupakan konstanta signifikan yang didominasi oleh konstanta diurnal. Nilai amplitudo tertinggi berada pada konstanta S2 dan M2 (semi-diurnal) sehingga menjelaskan mengapa tipe pasang surut yang didapatkan adalah tipe pasang surut harian ganda. Sedangkan 20 konstanta lainnya merupakan konstanta non-signifikan. Sementara itu hasil penghitungan bilangan Formzahl menunjukkan bahwa Teluk Davao juga bertipe pasang surut harian ganda dengan nilai sebesar 0,230493. Adapun tunggang pasang surut yang didapatkan dari hasil pengolahan dimana nilai maksimum adalah 2,27m dan nilai minimum adalah 0,12m. Sedangkan elevasi pasang surut maksimum yang didapatkan adalah 1,14m dan elevasi pasang surut minimum adalah 0,03m.
Continuous Fragmentation of Comet 157P/Tritton
Authors: Luu Jane , Jewitt David 
Published: December 2024

Abstract
We observed the split comet 157P/Tritton in 2022 October–November and 2024 January with the Nordic Optical Telescope. Our observations show that the splitting continued during the entire observing campaign. Fragmentation was associated with outbursts, consistent with the action of outgassing torques that spun up the nucleus and its fragments to the point of rotational instability. The outburst-fragmentation events can lead to a runaway process where the increasing spin rate, driven by outgassing torques, results in repeated mass loss until the sublimating body completely disintegrates.
The 10 pc Neighborhood of Habitable Zone Exoplanetary Systems: Threat Assessment from Stellar Encounters and Supernovae
Authors: Pyne Tisyagupta , Banyal Ravinder K. , Swastik C. , De Ayanabha 
Published: December 2024

Abstract
The habitability of a planet is influenced by both its parent star and the properties of its local stellar neighborhood. Potential threats to habitability from the local stellar environment mainly arise from two factors: cataclysmic events such as powerful stellar explosions and orbital perturbations induced by close stellar encounters. Among the 4500+ exoplanet-hosting stars, about 140+ are known to host planets in their habitable zones (HZs). In this study, we use Gaia Data Release 3 data to investigate the 10 pc stellar neighborhood of the 84 habitable zone systems (HZSs) closest to the Sun. We assess the possible risks that the local stellar environments of these HZSs pose to their habitability. In particular, we find that HD 165155 has a high stellar density around it, making it likely to experience at least one flyby encounter within a span of 5 Gyr. We also identified two high-mass stars (M ≥ 8 M
⊙) as potential progenitors of supernovae, which could threaten the long-term survivability of HZSs HD 48265 and TOI-1227. Further, to quantify the similarity between HZ stars and the Sun, as well as their respective 10 pc stellar environments, we employ various astrophysical parameters to define a solar similarity index and a neighborhood similarity index. Our analysis suggests that HD 40307 exhibits the closest resemblance to the solar system, while HD 165155 shows the least resemblance.
The Star-forming Main Sequence in JADES and CEERS at z > 1.4: Investigating the Burstiness of Star Formation
Authors: Clarke Leonardo , Shapley Alice E. , Sanders Ryan L. , Topping Michael W. , Brammer Gabriel B. , Bento Trinity , Reddy Naveen A. , Kehoe Emily 
Published: December 2024

Abstract
We have used public JWST/NIRSpec and JWST/NIRCam observations from the CEERS and JADES surveys in order to analyze the star-forming main sequence (SFMS) over the redshift range 1.4 ≤ z < 7. We calculate the star formation rates (SFRs) of the galaxy sample using three approaches: Balmer line luminosity, spectral energy distribution (SED) fitting, and UV luminosity. We find a larger degree of scatter about the SFMS using the Balmer-based SFRs compared to the UV-based SFRs. Because these SFR indicators are sensitive to star formation on different timescales, the difference in scatter may be evidence of bursty star formation histories in the early Universe. We additionally compare the Hα-to-UV luminosity ratio (L(Hα)/ν
L

ν,1600) for individual galaxies in the sample and find that 29%–52% of the ratios across the sample are poorly described by predictions from a smooth star formation history. Measuring the burstiness of star formation in the early Universe has multiple significant implications, such as deriving accurate physical parameters from SED fitting, explaining the evolution of the UV luminosity function, and providing constraints for subgrid models of feedback in simulations of galaxy formation and evolution.
Galaxy Spectroscopy without Spectra: Galaxy Properties from Photometric Images with Conditional Diffusion Models
Authors: Doorenbos Lars , Sextl Eva , Heng Kevin , Cavuoti Stefano , Brescia Massimo , Torbaniuk Olena , Longo Giuseppe , Sznitman Raphael , Márquez-Neila Pablo 
Published: December 2024

Abstract
Modern spectroscopic surveys can only target a small fraction of the vast amount of photometrically cataloged sources in wide-field surveys. Here, we report the development of a generative artificial intelligence (AI) method capable of predicting optical galaxy spectra from photometric broadband images alone. This method draws from the latest advances in diffusion models in combination with contrastive networks. We pass multiband galaxy images into the architecture to obtain optical spectra. From these, robust values for galaxy properties can be derived with any methods in the spectroscopic toolbox, such as standard population synthesis techniques and Lick indices. When trained and tested on 64 × 64 pixel images from the Sloan Digital Sky Survey, the global bimodality of star-forming and quiescent galaxies in photometric space is recovered, as well as a mass–metallicity relation of star-forming galaxies. The comparison between the observed and the artificially created spectra shows good agreement in overall metallicity, age, Dn4000, stellar velocity dispersion, and E(B − V) values. Photometric redshift estimates of our generative algorithm can compete with other current, specialized deep learning techniques. Moreover, this work is the first attempt in the literature to infer velocity dispersion from photometric images. Additionally, we can predict the presence of an active galactic nucleus up to an accuracy of 82%. With our method, scientifically interesting galaxy properties, normally requiring spectroscopic inputs, can be obtained in future data sets from large-scale photometric surveys alone. The spectra prediction via AI can further assist in creating realistic mock catalogs.
Infrared Band Strengths and Other Properties of Three Interstellar Compounds—Amorphous Isocyanic Acid, Formaldehyde, and Formic Acid
Authors: Hudson Reggie L. , Yarnall Yukiko Y. , Gerakines Perry A. 
Published: December 2024

Abstract
Infrared (IR) spectral features of interstellar and solar system ices have been attributed to solid organic and inorganic compounds for over 50 yr, but in many cases the laboratory IR data needed to fully quantify such work have never been published, forcing researchers to rely on assumptions about gas- or liquid-phase measurements to interpret data for ices. Here, we report the first mid-IR intensity measurements for isocyanic acid (HNCO) ices that are free of such assumptions, providing new results for use by both observational and laboratory astrochemists. We also report similar new IR data for both formaldehyde (H2CO) and formic acid (HCOOH), which have been discussed in the astrochemical literature for decades, but again without adequate laboratory data to help quantify observational results. Densities and refractive indices of HNCO, H2CO, and HCOOH as amorphous ices also are reported. Two applications of the new H2CO work are presented, the first vapor-pressure measurements of solid H2CO, along with an enthalpy of sublimation, at 100 to 109 K and a set of IR intensities of H2CO in H2O + H2CO ices. Band strengths, absorption coefficients, and optical constants are calculated for all three compounds. Extensive comparisons are made to older results, which are not recommended for future use.
Multiple Components of the Outflow in the Protostellar System HH 212: Outer Outflow Shell, Rotating Wind, Shocked Wind, and Jet
Authors: López-Vázquez J. A. , Lee Chin-Fei , Shang Hsien , Cabrit Sylvie , Krasnopolsky Ruben , Codella Claudio , Liu Chun-Fan , Podio Linda , Dutta Somnath , Murphy A. , Wiseman Jennifer 
Published: December 2024

Abstract
We present the Atacama Large Millimeter/submillimeter Array Band 7 observations of the CO (J = 3−2) line emission of the protostellar system HH 212 at ∼24 au spatial resolution and compare them to those of the SiO (J = 8−7) and SO (J = 8−7) line emission reported in the literature. We find that the CO line traces four distinct regions: (1) an outer outflow shell, (2) a rotating wind region between the SiO and CO shells, (3) the shocked and wide-angle inner X-wind inside a SiO shell, and (4) the jet. The origin of the CO outer outflow shell could be associated with the entrained material of the envelope, or an extended disk wind. The rotating wind, which is shocked, is launched from a radius of 9–15 au, slightly exterior to that of the previously detected SO shell, which marks the boundary where the wide-angle X-wind is interacting with and shocking the disk wind. Additionally, the SO is found to be mixed with the CO emission within the thick and extended rotating wind region. The large-scale CO-shocked wind coexists with the SO emission near the upper portion of the inner shocked region converged on top of the inner SiO knots. The CO jet is traced by a chain of knots with roughly equal intervals, exhibiting quasiperiodicity, as reported in other jets in the literature.
Mergers, Radio Jets, and Quenching Star Formation in Massive Galaxies: Quantifying Their Synchronized Cosmic Evolution and Assessing the Energetics
Authors: Heckman Timothy M. , Roy Namrata , Best Philip N. , Kondapally Rohit 
Published: December 2024

Abstract
The existence of a population of massive quiescent galaxies with little to no star formation poses a challenge to our understanding of galaxy evolution. The physical process that quenched the star formation in these galaxies is debated, but the most popular possibility is that feedback from supermassive black holes lifts or heats the gas that would otherwise be used to form stars. In this paper, we evaluate this idea in two ways. First, we compare the cumulative growth in the cosmic inventory of the total stellar mass in quiescent galaxies to the corresponding growth in the amount of kinetic energy carried by radio jets. We find that these two inventories are remarkably well-synchronized, with about 50% of the total amounts being created in the epoch from z ≈ 1 to 2. We also show that these agree extremely well with the corresponding growth in the cumulative number of major mergers that result in massive (>1011
M
ʘ) galaxies. We therefore argue that major mergers trigger the radio jets and also transform the galaxies from disks to spheroids. Second, we evaluate the total amount of kinetic energy delivered by jets and compare it to the baryonic binding energy of the galaxies. We find the jet kinetic energy is more than sufficient to quench star formation, and the quenching process should be more effective in more massive galaxies. We show that these results are quantitatively consistent with recent measurements of the Sunyaev–Zel’dovich effect seen in massive galaxies at z ≈ 1.
Detailed Calculations of the Efficiency of Planetesimal Accretion in the Core-accretion Model. III. The Contribution of Planetesimals beyond Saturn
Authors: Haghighipour Nader , Podolak Morris , Podolak Esther 
Published: December 2024

Abstract
Continuing our initiative on advancing the calculations of planetesimal accretion in the core-accretion model, we present here the results of our recent study of the contributions of planetesimals around and beyond the orbit of Saturn. In our first two papers, where our focus was on the effects of the Sun and Saturn, the initial distribution of planetesimals was limited to the regions around the accretion zone of a growing Jupiter. In this paper, we expanded that distribution to regions beyond the accretion zone of Saturn. We integrated the orbits of a large ensemble of planetesimals and studied the rate of their capture by the growing proto-Jupiter. In order to be consistent with our previous studies, we did not consider the effect of the nebular gas. Results demonstrated that the exterior planetesimals, especially those beyond 8 au, have only slight contributions to the growth and metallicity of the growing Jupiter. The final mass and composition of this planet is mainly due to the planetesimals inside and around its accretion zone. Our study shows that although the rate of capture varies slightly by the size and composition of planetesimals, in general, the final results are independent of the size and material of these bodies. Results also pointed to a new finding: the rate of accretion follows the same trend as that of the evolution of Jupiter’s envelope, with the largest accretion occurring during the envelope’s collapse. We present details of our analysis and discuss the implications of its results.
An Eccentric Binary with a Misaligned Circumbinary Disk
Authors: Hu 胡 Zhecheng 哲程 , Zhu 祝 Wei 伟 , Dai 戴 Fei 飞 , Chen 陈 Ping 平 , Huang 黄 Yang 样 , Fang 房 Min 敏 , Post Richard S. 
Published: December 2024

Abstract
We present spectroscopic and photometric observations of Bernhard-2, which was previously identified as a candidate system that hosts a misaligned circumbinary disk. Our spectroscopic measurements confirm that Bernhard-2 indeed contains an eccentric (e = 0.69 ± 0.08) binary and thus that the periodic variability in the photometric light curve is best explained by the occultation by the misaligned circumbinary disk. By modeling the spectral energy distributions at different phases, we infer the masses of the two binary components to be ∼1.1 M
⊙ and ∼0.9 M
⊙, respectively. The system age is determined to be ≲20 Myr by combining the stellar isochrone model with lithium abundance. Our new photometric observations show clear deviations from the model prediction based on the archival data, suggesting ongoing precession of the circumbinary disk. The Hα line of Bernhard-2 also shows an inverse P-Cygni profile at epochs close to the pericenter passage, which could be attributed to the pulsed accretion around the pericenter. Bernhard-2 therefore closely resembles the well-studied KH 15D system. Further detailed observations and studies of such rare systems can provide useful information about disk physics and evolution.
Theoretical Studies on the Evolution of Solar Filaments in Response to New Emerging Flux
Authors: Chen Yuhao , Hu Jialiang , Cheng Guanchong , Ye Jing , Mei Zhixing , Shen Chengcai , Lin Jun 
Published: December 2024

Abstract
New emerging flux (NEF) has long been considered a mechanism for solar eruptions, but the detailed process remains an open question. In this work, we explore how NEF drives a coronal magnetic configuration to erupt. This configuration is created by two magnetic sources of strengths M and S embedded in the photosphere, one electric-current-carrying flux rope (FR) floating in the corona, and an electric current induced on the photospheric surface by the FR. The source M is fixed, accounting for the initial background field, and S changes, playing the role of NEF. We introduce the channel function C to forecast the overall evolutionary behavior of the configuration. The location, polarity, and strength of NEF govern the evolutionary behavior of the FR before eruption. In the case of ∣S/M∣ < 1, with reconnection occurring between new and old fields, the configuration in equilibrium evolves to the critical state, invoking the catastrophe. In this case, if the polarities of the new and old fields are opposite, reconnection occurs as NEF is close to the FR, and if the polarities are the same, reconnection happens as NEF appears far from the FR. With different combinations of the relative polarity and the location, the evolutionary behavior of the system gets complex, and the catastrophe may not occur. If ∣S/M∣ > 1 and the two fields have opposite polarity, the catastrophe always takes place, but if the polarities are the same, the catastrophe occurs only as NEF is located far from the FR; otherwise, the evolution ends up either with a failed eruption or without a catastrophe at all.
Comprehensive Study of Near-Earth Asteroid 2024 MK: Testing Planetary Encounters as a Source for Surface Refreshing
Authors: McGraw Lauren E. , Thomas Cristina A. , Lister Tim A. , Williams Becky J. , Rivkin Andy S. , Holler Bryan , Young Leslie A. 
Published: December 2024

Abstract
Near-Earth object 2024 MK was discovered on 2024 June 16, less than 2 weeks before it made a sub-lunar-distance close approach. This close approach provided an ideal opportunity to determine how planetary encounters affect asteroid surfaces in preparation for the numerous missions to (99942) Apophis during its close approach in 2029. We collected spectroscopic data before and after its close approach to determine if planetary encounters induce spectral changes due to surface refreshing. We used NASA’s Infrared Telescope Facility’s (IRTF) near-infrared spectrometer SpeX prism mode (0.7–2.5 μm) to observe 2024 MK pre and postapproach. We also observed the asteroid before its close approach using Las Cumbres Observatory’s FLOYDS visible spectrometer and after its close approach using IRTF’s SpeX long-wavelength cross-dispersed short grating mode, resulting in full spectral coverage from 0.32 to 4.2 μm. 2024 MK is an S-type asteroid that is compositionally most analogous to an L-ordinary chondrite. Spectral analysis of the 3 μm region indicates no surficial water or hydroxide within the level of noise. Band parameter analysis of the pre and postapproach data shows the planetary encounter did not induce any significant spectral changes, suggesting that surface refreshing did not occur on a measurable scale. Similar studies of other targets at smaller encounter distances are required to determine if the lack of spectral changes on 2024 MK indicates it was not close enough to Earth to affect its surface or if the spectral similarity pre and postapproach instead indicates planetary encounters do not cause surface refreshing.
Observations of Uranus at High Phase Angle as Seen by New Horizons
Authors: Hasler Samantha N. , Mayorga L. C. , Grundy William M. , Simon Amy A. , Benecchi Susan D. , Howett Carly J. A. , Protopapa Silvia , Hammel Heidi B. , Wenkert Daniel D. , Stern S. Alan , Singer Kelsi N. , Porter Simon B. , Brandt Pontus C. , Parker Joel W. , Verbiscer Anne J. , Spencer John R. ,   The New Horizons Planetary Science Theme Team
Published: December 2024

Abstract
We present flux measurements of Uranus observed at phase angles of 43.°9, 44.°0, and 52.°4 by the Multispectral Visible Imaging Camera on the New Horizons spacecraft during 2023, 2010, and 2019, respectively. New Horizons imaged Uranus at a distance of about 24–70 au (2023) in four color filters, with bandpasses of 400–550 nm, 540–700 nm, 780–975 nm, and 860–910 nm. High-phase-angle observations are of interest for studying the energy balance of Uranus, constraining the atmospheric scattering behavior, and understanding the planet as an analog for ice giant exoplanets. The new observations from New Horizons provide access to a wider wavelength range and different season compared with previous observations from the Voyager spacecraft. We performed aperture photometry on the New Horizons observations of Uranus to obtain its brightness in each photometric band. The photometry suggests that Uranus may be darker than predicted by a Lambertian phase curve in the blue and red filters. Comparison to simultaneous low-phase Hubble WFC3 and ground-based community-led observations indicates a lack of large-scale features at full phase that would introduce variation in the rotational light curve. The New Horizons reflectance in the blue (492 nm) and red (624 nm) filters does not exhibit statistically significant variation and is consistent with the expected error bars. These results place new constraints on the atmospheric model of Uranus and its reflectivity. The observations are analogous to those from future exoplanet direct-imaging missions, which will capture unresolved images of exoplanets at partial phases. These results will serve as a “ground truth” with which to interpret exo-ice-giant data.