bluuebunny/crossref_metadata_2025_split huggingface dataset:
A Volume-limited Radio Search for Magnetic Activity in 140 Exoplanets with the Very Large Array
Authors: Ortiz Ceballos Kevin N. , Cendes Yvette , Berger Edo , Williams Peter K. G. 
Published: August 2024

Abstract
We present results from a search for radio emission in 77 stellar systems hosting 140 exoplanets, predominantly within 17.5 pc using the Very Large Array (VLA) at 4–8 GHz. This is the largest and most sensitive search to date for radio emission in exoplanetary systems in the GHz frequency range. We obtained new observations of 58 systems and analyzed archival observations of an additional 19 systems. Our choice of frequency and volume limit is motivated by radio detections of ultracool dwarfs (UCDs), including T dwarfs with masses at the exoplanet threshold of ∼13 M
J. Our surveyed exoplanets span a mass range of ≈10−3–10 M
J and semimajor axes of ≈10−2–10 au. We detect a single target—GJ 3323 (M4) hosting two exoplanets with minimum masses of 2 and 2.3 M
⊕—with a circular polarization fraction of ≈40%; the radio luminosity agrees with its known X-ray luminosity and the Güdel–Benz relation for stellar activity suggesting a likely stellar origin, but the high circular polarization fraction may also be indicative of star–planet interaction. For the remaining sources our 3σ upper limits are generally L

ν
≲ 1012.5 erg s−1 Hz−1, comparable to the lowest radio luminosities in UCDs. Our results are consistent with previous targeted searches of individual systems at GHz frequencies while greatly expanding the sample size. Our sensitivity is comparable to predicted fluxes for some systems considered candidates for detectable star–planet interaction. Observations with future instruments such as the Square Kilometre Array and Next-Generation VLA will be necessary to further constrain emission mechanisms from exoplanet systems at GHz frequencies.
JWST-TST DREAMS: Nonuniform Dayside Emission for WASP-17b from MIRI/LRS
Authors: Valentine Daniel , Wakeford Hannah R. , Challener Ryan C. , Batalha Natasha E. , Lewis Nikole K. , Grant David , Mullens Elijah , Alderson Lili , Goyal Jayesh , MacDonald Ryan J. , May Erin M. , Seager Sara , Stevenson Kevin B. , Valenti Jeff A. , Allen Natalie H. , Espinoza Néstor , Glidden Ana , Gressier Amélie , Huang Jingcheng , Lin Zifan , Long Douglas , Louie Dana R. , Clampin Mark , Perrin Marshall , van der Marel Roeland P. , Mountain C. Matt 
Published: August 2024

Abstract
We present the first spectroscopic characterization of the dayside atmosphere of WASP-17b in the mid-infrared using a single JWST MIRI/LRS eclipse observation. From forward-model fits to the 5–12 μm emission spectrum, we tightly constrain the heat redistribution factor of WASP-17b to be 0.92 ± 0.02 at the pressures probed by this data, indicative of inefficient global heat redistribution. We also marginally detect a supersolar abundance of water, consistent with previous findings for WASP-17b, but note our weak constraints on this parameter. These results reflect the thermodynamically rich but chemically poor information content of MIRI/LRS emission data for high-temperature hot Jupiters. Using the eclipse mapping method, which utilizes the signals that the spatial emission profile of an exoplanet imprints on the eclipse light curve during ingress/egress due to its partial occultation by the host star, we also construct the first eclipse map of WASP-17b, allowing us to diagnose its multidimensional atmospheric dynamics for the first time. We find a day–night temperature contrast of order 1000 K at the pressures probed by this data, consistent with our derived heat redistribution factor, along with an eastward longitudinal hotspot offset of

18.7

−
3.8

+
11.1
◦

, indicative of the presence of an equatorial jet induced by day–night thermal forcing being the dominant redistributor of heat from the substellar point. These dynamics are consistent with general circulation model predictions for WASP-17b. This work is part of a series of studies by the JWST Telescope Scientist Team, in which we use Guaranteed Time Observations to perform Deep Reconnaissance of Exoplanet Atmospheres through Multi-instrument Spectroscopy.
Archetype-based Redshift Estimation for the Dark Energy Spectroscopic Instrument Survey
Authors: Anand Abhijeet , Guy Julien , Bailey Stephen , Moustakas John , Aguilar J. , Ahlen S. , Bolton A. S. , Brodzeller A. , Brooks D. , Claybaugh T. , Cole S. , de la Macorra A. , Dey Biprateep , Fanning K. , Forero-Romero J. E. , Gaztañaga E. , Gontcho A Gontcho S. , Gutierrez G. , Honscheid K. , Howlett C. , Juneau S. , Kirkby D. , Kisner T. , Kremin A. , Lambert A. , Landriau M. , Le Guillou L. , Manera M. , Meisner A. , Miquel R. , Mueller E. , Niz G. , Palanque-Delabrouille N. , Percival W. J. , Poppett C. , Prada F. , Raichoor A. , Rezaie M. , Rossi G. , Sanchez E. , Schlafly E. F. , Schlegel D. , Schubnell M. , Sprayberry D. , Tarlé G. , Warner C. , Weaver B. A. , Zhou R. , Zou H. 
Published: August 2024

Abstract
We present a computationally efficient galaxy archetype-based redshift estimation and spectral classification method for the Dark Energy Survey Instrument (DESI) survey. The DESI survey currently relies on a redshift fitter and spectral classifier using a linear combination of principal component analysis–derived templates, which is very efficient in processing large volumes of DESI spectra within a short time frame. However, this method occasionally yields unphysical model fits for galaxies and fails to adequately absorb calibration errors that may still be occasionally visible in the reduced spectra. Our proposed approach improves upon this existing method by refitting the spectra with carefully generated physical galaxy archetypes combined with additional terms designed to absorb data reduction defects and provide more physical models to the DESI spectra. We test our method on an extensive data set derived from the survey validation (SV) and Year 1 (Y1) data of DESI. Our findings indicate that the new method delivers marginally better redshift success for SV tiles while reducing catastrophic redshift failure by 10%–30%. At the same time, results from millions of targets from the main survey show that our model has relatively higher redshift success and purity rates (0.5%–0.8% higher) for galaxy targets while having similar success for QSOs. These improvements also demonstrate that the main DESI redshift pipeline is generally robust. Additionally, it reduces the false-positive redshift estimation by 5%−40% for sky fibers. We also discuss the generic nature of our method and how it can be extended to other large spectroscopic surveys, along with possible future improvements.
Concurrent Particle Acceleration and Pitch-angle Anisotropy Driven by Magnetic Reconnection: Ion-electron Plasmas
Authors: Comisso Luca 
Published: August 2024

Abstract
Particle acceleration and pitch-angle anisotropy resulting from magnetic reconnection are investigated in highly magnetized ion-electron plasmas. By means of fully kinetic particle-in-cell simulations, we demonstrate that magnetic reconnection generates anisotropic particle distributions

f

s

∣
cos
α
∣
,
ε

, characterized by broken power laws in the particle energy spectrum f

s
(ε) ∝ ε
−p
and pitch angle

〈

sin

2

α
〉
∝

ε

m

. The characteristics of these distributions are determined by the relative strengths of the magnetic field’s guide and reconnecting components (B

g
/B
0) and the plasma magnetization (σ
0). Below the injection break energy ε
0, ion and electron energy spectra are extremely hard (p
< ≲ 1) for any B

g
/B
0 and σ
0 ≳ 1, while above ε
0 the spectral index steepens (p
> ≳ 2), displaying high sensitivity to both B

g
/B
0 and σ
0. The pitch angle displays power-law ranges with negative slopes (m
<) below and positive slopes (m
>) above

ε

min
α

, steepening with increasing B

g
/B
0 and σ
0. The ratio B

g
/B
0 regulates the redistribution of magnetic energy between ions (ΔE

i
) and electrons (ΔE

e
), with ΔE

i
≫ ΔE

e
for B

g
/B
0 ≪ 1, ΔE

i
∼ ΔE

e
for B

g
/B
0 ∼ 1, and ΔE

i
≪ ΔE

e
for B

g
/B
0 ≫ 1, with ΔE

i
/ΔE

e
approaching unity when σ
0 ≫ 1. The anisotropic distribution of accelerated particles results in an optically thin synchrotron power spectrum F

ν
(ν) ∝ ν
(2−2p+m)/(4+m) and a linear polarization degree Πlin = (p + 1)/(p + 7/3 + m/3) for a uniform magnetic field. Pitch-angle anisotropy also induces temperature anisotropy and eases synchrotron cooling, along with producing beamed radiation aligned with the magnetic field, which is potentially responsible for rapid frequency-dependent variability.
Constraining the Number Density of the Accretion Disk Wind in Hercules X-1 Using Its Ionization Response to X-Ray Pulsations
Authors: Kosec P. , Rogantini D. , Kara E. , Canizares C. R. , Fabian A. C. , Pinto C. , Psaradaki I. , Staubert R. , Walton D. J. 
Published: August 2024

Abstract
X-ray binaries are known to launch powerful accretion disk winds that can have a significant impact on the binary systems and their surroundings. To quantify the impact and determine the launching mechanisms of these outflows, we need to measure the wind plasma number density, an important ingredient in the theoretical disk wind models. While X-ray spectroscopy is a crucial tool for understanding the wind properties, such as their velocity and ionization, in nearly all cases, we lack the signal-to-noise ratio to constrain the plasma number density, weakening the constraints on the outflow location and mass outflow rate. We present a new approach to determining this number density in the X-ray binary Hercules X-1, by measuring the speed of the wind ionization response to the time-variable illuminating continuum. Hercules X-1 is powered by a highly magnetized neutron star, pulsating with a period of 1.24 s. We show that the wind number density in Hercules X-1 is sufficiently high to respond to these pulsations by modeling the ionization response with the time-dependent photoionization model tpho. We then perform a pulse-resolved analysis of the best-quality XMM-Newton observation of Hercules X-1 and directly detect the wind response, confirming that the wind density is at least 1012 cm−3. Finally, we simulate XRISM observations of Hercules X-1 and show that they will allow us to accurately measure the number density at different locations within the outflow. With XRISM, we will rule out ∼3 orders of magnitude in density parameter space, constraining the wind mass outflow rate, energetics, and its launching mechanism.
Robust r-process Nucleosynthesis beyond Lanthanides in the Common Envelop Jet Supernovae
Authors: Jin Shilun , Soker Noam 
Published: August 2024

Abstract
The common envelop jet supernovae (CEJSNe) r-process scenario has been proposed as an r-process nucleosynthesis site in the past decade. Jets launched by a neutron star that spirals in inside the core of a red supergiant star in a common envelope evolution supply the proper conditions for forming elements heavier than iron through the rapid neutron-capture process. The present work initially unveils the r-process abundance patterns that result from the density profile in the relatively long-lived jets. The results indicate that the expansion profile unique to the CEJSN scenario can produce the largest ratio of the third r-process peak elements to lanthanides among current r-process scenarios and, in addition, can form quite an amount of lanthanides, about 1% of matters above the first peak, in a single event. The comparison of the ratio of the third-peak elements to the lanthanides with several observed r-enhanced metal-poor stars and with other r-process scenarios suggests that a high mass of third-peak elements is anticorrelated with a high fraction of lanthanides, both in observations and theory. The CEJSN-like scenario plays a significant role in this conclusion since it reproduces the observational features of some particular r-enhanced metal-poor stars where other r-process scenarios encounter problems. Due to the formation of extremely heavy elements, the CEJSN also offers a credible estimation of the age of the most actinide-boosted star by cosmochronometry.
Revealing the Fate of Exoplanet Systems: Asteroseismic Identification of Host Star in the Red Clump or Red Giant Branch
Authors: Lin Wen-Xu , Qian Sheng-Bang , Zhu Li-Ying 
Published: August 2024

Abstract
Determining the evolutionary stage of stars is crucial for understanding the evolution of exoplanetary systems. In this context, red giant branch (RGB) and red clump (RC) stars, which formed at stages in the later evolution of stars situated before and after the helium flash, harbor critical clues to unveiling the evolution of planets. The first step in revealing these clues is to confirm the evolutionary stage of the host stars through asteroseismology. However, up to now, host stars confirmed to be RGB or RC stars are extremely rare. In this investigation, we present a comprehensive asteroseismic analysis of two evolved stars, HD 120084 and HD 29399, known to harbor exoplanets, using data from the Transiting Exoplanet Survey Satellite. We have discovered for the first time that HD 120084 is an RC star in the helium-core-burning phase, and confirmed that HD 29399 is an RGB star in the hydrogen-shell burning phase. Through the precise measurement of asteroseismic parameters such as

ν

max

, Δν, and ΔΠ1, we have determined the evolutionary states of these stars and derived their fundamental stellar parameters. The significance of this study lies in the application of automated techniques to measure asymptotic period spacings in red giants, which provides critical insights into the evolutionary outcomes of exoplanet systems. We demonstrate that asteroseismology is a potent tool for probing the internal structures of stars, thereby offering a window into the past and future dynamics of planetary orbits. The presence of a long-period giant planet orbiting HD 120084, in particular, raises intriguing questions about the potential engulfment of inner planets during the host star’s expansion, a hypothesis that warrants further investigation.
Bambara groundnut landraces response and tolerance to drought stress: A meta-analysis
Authors: Mabitsela Mosima M. , Phiri Ethel E. , Booysen Marthinus J. , Mavengahama Sydney 
Published: August 2024

Background: Drought stress severely limits agricultural productivity. Bambara groundnut, an underutilised legume, shows promise for its resilience to harsh environments, particularly drought. Drought duration and manipulation type have been used to evaluate the response of Bambara groundnut to drought stress. Although studies have explored the effects of drought duration and manipulation on Bambara groundnut, an understanding of the legume’s response to drought stress remains inadequate.Aim: This meta-analysis assessed Bambara groundnut’s response to different drought durations (long-term, medium-term, short-term) and manipulation types (constant, dry-and-rewetting, intermittent).Setting: The study integrates data from multiple independent studies to evaluate how various drought durations and manipulations affect Bambara groundnut.Methods: A systematic review and meta-analysis of studies examining drought’s effects on Bambara groundnut were conducted. Data from qualifying studies were extracted and statistically analysed to quantify drought’s impact on various physiological and yield parameters.Results: Drought stress significantly reduced yield (–10.22), stomatal conductance (–8.04), and pod number (–4.20). Short-term and medium-term droughts had a greater negative impact than long-term droughts. Intermittent drought did not affect biomass, plant height, leaf number, and chlorophyll content, while dry-and-rewetting cycles did not affect seed number.Conclusion: Based on the meta-analysis, future drought scenarios are predicted to negatively impact Bambara groundnut productivity, surpassing the challenges posed by current drought conditions.Contribution: This study emphasises the importance of developing strategies to enhance the resilience of indigenous crops, such as Bambara groundnut to drought, crucial for ensuring future food security in the face of changing climate patterns.
Factors influencing data quality in routine health information systems in Maridi county, South Sudan
Authors: Morris Lubang D. , Nyongesa Margaret W. , Sokiri Tobijo D. 
Published: August 2024

Background: Health system planning and monitoring rely on routine data collection, analysis and utilisation. However, underdeveloped countries need more data for decision-making. South Sudan’s data management framework only partially functions, with delayed data collection and inaccurate data. The study examined the factors affecting data quality in Maridi County, South Sudan, aiming to improve resource forecasting and equitable health service delivery.Objective: The study sought to identify the obstacles and opportunities for improving data quality in health information systems (HIS) in Maridi County, Western Equatoria State, South Sudan.Methods: A cross-sectional study involving 106 respondents was conducted on 12 healthcare facilities in Maridi County. Statistical Package for the Social Sciences (SPSS) version 25 was used for descriptive, factor and thematic analysis to understand data quality, focussing on behavioural, organisational and technical aspects.Result: The study revealed that insufficient motivation, negative staff attitudes, excessive workloads, a lack of cooperation, personnel insufficiency, inadequate supervision, feedback and training influenced data quality. These factors were interrelated, with over 50% of variables showing weak to strong correlations. Set of standard indicators correlated with the presence of standard data collection tools (r = 0.51). Regular feedback from the County Health Department linked with completeness (r = 0.63) and the training of personnel on health management information systems (HMIS) and completeness resulted in moderate association (r = 0.488).Conclusion: Staff motivation, optimal staffing, training, regular feedback, and continuous supervision are crucial for maintaining the appropriate skill set for data quality.Contribution: Data quality can be achieved when standard tools and human resources are maintained and are evenly distributed.
Holiness and sustainable social transformation among neo-Pentecostal prophets in South Africa
Authors: Banda Collium 
Published: August 2024

This article critically examines how African neo-Pentecostal prophets (ANPPs) address the pervasive issues of uncertainty and hopelessness in South Africa through controversial prophetic practices that challenge conventional notions of divine holiness. In light of South Africa’s persistent state of uncertainty, despite its status as one of the most progressive countries in Africa, do ANPPs inspire and support actions that can transform this adverse context into a positive and sustainable one? The question is addressed by first describing how South Africa remains a context of uncertainty, even though it is one of the most progressive countries in Africa. The article then discusses the pivotal role of ‘holiness’ in fostering sustainable social transformation. Thereafter, it examines the ANPPs’ attempts to transform the context of uncertainty and hopelessness in the country, analysing how the perceived unholiness in their activities obstructs sustainability in these efforts. Finally, the article concludes by affirming the importance of holiness in the quest for sustainable social transformation in South Africa.Intradisciplinary and/or interdisciplinary implications: The article combines frameworks from sustainable development and systematic theology to call ANPPs to reform their religious practices in alignment with God’s holiness, in order to make meaningful contributions to the contemporary quest for sustainable transformation and development in South Africa.
Correlation between non-alcoholic fatty liver disease and metabolic parameters in persons with newly diagnosed type 2 diabetes mellitus
Authors: Mukherjee Supriyo , Mukherjee Sushmita , Shing Kwok Chun , Phillips Anne 
Published: August 2024

BACKGROUND
There are limited studies investigating the association between type 2 diabetes mellitus (T2DM) and non-alcoholic fatty liver disease (NAFLD) in the region of Bihar, India.
AIM
To estimate the prevalence of NAFLD in persons with newly diagnosed T2DM in the population of North Bihar, India.
METHODS
This single centre cross-sectional study was undertaken in the Research Centre for Diabetes Hypertension and Obesity, Samastipur, Bihar, India. Data were collected from persons newly diagnosed with T2DM or those diagnosed within 6 months of when the study was conducted between December 2022 to May 2023.
RESULTS
A total of 148 people with newly diagnosed T2DM were included (median age 47 years, 46.6% female) and 109 patients with liver disease on ultrasound evaluation. The persons with liver disease consumed more fats and oils (88.1% vs 74.4%, P = 0.042) and they had significantly greater body mass index (27.4 vs 23.0, P < 0.001), waist circumference (37 vs 33, P < 0.001), and waist-to-hip ratio (1.00 vs 0.70, P = 0.025). Females were associated with greater liver disease [odds ratio (OR): 3.09, 95% confidence interval (CI): 1.09-8.80, P = 0.32]. Waist circumference (OR: 1.42, 95%CI: 1.22-1.66, P < 0.001) and low-density lipoprotein cholesterol (OR: 1.01, 95%CI: 1.01-1.02, P = 0.048) were associated with any liver disease. The factors most associated with grade 2/3 liver disease was right upper quadrant pain or heaviness (OR: 5.22, 95%CI: 1.40-19.41, P = 0.14), greater income (OR: 3.58, 95%CI: 1.28-10.04, P = 0.015) and waist circumference (OR: 1.31, 95%CI: 1.02-1.69, P = 0.036).
CONCLUSION
NAFLD is common in new/recently diagnosed T2DM and disease burden is high and common among patients who are either high consumers of fats and oils or have obesity-associated markers.
PEMANFAATAN APLIKASI iPUSNAS DALAM MEMENUHI KEBUTUHAN INFORMASI MAHASISWA ILMU PERPUSTAKAAN UIN SUMATERA UTARA
Authors: Gulo Elsa Karenina , Fathurrahman Muslih 
Published: August 2024

Cara orang mendapatkan informasi telah berubah karena teknologi informasi dan komunikasi (TIK), termasuk perpustakaan yang kini beralih menjadi digital. iPusnas adalah salah satu aplikasi perpustakaan digital yang ada di Indonesia, yang dirancang untuk memudahkan akses informasi bagi masyarakat, termasuk mahasiswa. Pendekatan deskriptif digunakan dalam penelitian kualitatif ini. 10 mahasiswa ilmu perpustakaan UIN Sumatera utara diwawancarai guna mengumpulkan data untuk memahami pemanfaatan iPusnas dan faktor-faktor yang mempengaruhinya. iPusnas dinilai mudah digunakan dan bermanfaat untuk kebutuhan akademik mahasiswa. Namun, terdapat beberapa kendala seperti kesalahan sistem, koleksi yang kurang lengkap, tidak adanya notifikasi pesan chatting, dan batas peminjaman buku yang rendah. Kendala-kendala ini mempengaruhi efektivitas penggunaan aplikasi oleh mahasiswa. iPusnas memiliki potensi besar untuk mendukung kebutuhan akademik mahasiswa, namun belum optimal digunakan. Diperlukan peningkatan dalam sistem teknis, perluasan koleksi, penambahan notifikasi pesan chatting, dan revisi batas peminjaman buku untuk meningkatkan pemanfaatan aplikasi ini.