bluuebunny/crossref_metadata_2025_split huggingface dataset:
UNCOVER NIRSpec/PRISM Spectroscopy Unveils Evidence of Early Core Formation in a Massive, Centrally Dusty Quiescent Galaxy at z
spec = 3.97
Authors: Setton David J. , Khullar Gourav , Miller Tim B. , Bezanson Rachel , Greene Jenny E. , Suess Katherine A. , Whitaker Katherine E. , Antwi-Danso Jacqueline , Atek Hakim , Brammer Gabriel , Cutler Sam E. , Dayal Pratika , Feldmann Robert , Fujimoto Seiji , Furtak Lukas J. , Glazebrook Karl , Goulding Andy D. , Kokorev Vasily , Labbe Ivo , Leja Joel , Ma 马 Yilun 逸伦 , Marchesini Danilo , Nanayakkara Themiya , Pan Richard , Price Sedona H. , Siegel Jared C. , Shipley Heath , Weaver John R. , van Dokkum Pieter , Wang 王 Bingjie 冰洁 , Williams Christina C. 
Published: October 2024

Abstract
We report the spectroscopic confirmation of a massive (

log
(

M

⋆

/

M

⊙

)
=
10.34

±

0.07

0.06

), Hubble Space Telescope–dark (m
F150W − m
F444W = 3.6) quiescent galaxy at z
spec = 3.97 in the UNCOVER survey. NIRSpec/PRISM spectroscopy and a nondetection in deep Atacama Large Millimeter/submillimeter Array imaging surprisingly reveals that the galaxy is consistent with a low (<10 M
⊙ yr−1) star formation rate (SFR) despite evidence for moderate dust attenuation. The F444W image is well modeled with a two-component Sérsic fit that favors a compact, r

e
∼ 200 pc, n ∼ 2.9 component and a more extended, r

e
∼ 1.6 kpc, n ∼ 1.7 component. The galaxy exhibits strong color gradients: the inner regions are significantly redder than the outskirts. Spectral energy distribution models that reproduce both the red colors and low SFR in the center of UNCOVER 18407 require both significant (A

v
∼ 1.4 mag) dust attenuation and a stellar mass-weighted age of 900 Myr, implying 50% of the stars in the core already formed by z = 7.5. Using spatially resolved annular mass-to-light measurements enabled by the galaxy’s moderate magnification (

μ
=
2.12

±

0.01

0.05

) to reconstruct a radial mass profile from the best-fitting two-component Sérsic model, we infer a total mass-weighted

r

eff

=
0.74

±

0.17

0.22

kpc and log

(

Σ

1

kpc

[

M
⊙

kpc

-
2

]
)
=
9.65

±
0.15
0.12

. The early formation of a dense, low SFR, and dusty core embedded in a less attenuated stellar envelope suggests an evolutionary link between the earliest-forming massive galaxies and their elliptical descendants. Furthermore, the disparity between the global, integrated dust properties and the spatially resolved gradients highlights the importance of accounting for radially varying stellar populations when characterizing the early growth of galaxy structure.
Deriving the Interaction Point between a Coronal Mass Ejection and High-speed Stream: A Case Study
Authors: Remeshan Akshay Kumar , Dumbović Mateja , Temmer Manuela 
Published: October 2024

Abstract
We analyze the interaction between an interplanetary coronal mass ejection (ICME) detected in situ at the L1 Lagrange point on 2016 October 12 with a trailing high-speed stream (HSS). We aim to estimate the region in the interplanetary (IP) space where the interaction happened/started using a combined observational-modeling approach. We use minimum variance analysis (MVA) and the Walen test to analyze possible reconnection exhaust at the interface of ICME and HSS. We perform a graduated cylindrical shell reconstruction of the CME to estimate the geometry and source location of the CME. Finally, we use a two-step drag-based model (DBM) model to estimate the region in IP space where the interaction took place. The magnetic obstacle observed in situ shows a fairly symmetric and undisturbed structure and shows the magnetic flux, helicity, and expansion profile/speed of a typical ICME. The MVA together with the Walen test, however, confirms reconnection exhaust at the ICME–HSS boundary. Thus, in situ signatures are in favor of a scenario where the interaction is fairly recent. The trailing HSS shows a distinct velocity profile which first reaches a semi-saturated plateau with an average velocity of 500 km s−1 and then saturates at a maximum speed of 710 km s−1. We find that the HSS's interaction with the ICME is influenced only by this initial plateau. The results of the two-step DBM suggest that the ICME has started interacting with the HSS close to Earth (∼0.81 au), which compares well with the deductions from in situ signatures.
How Landmass Distribution Influences the Atmospheric Dynamics of Tidally Locked Terrestrial Exoplanets
Authors: Sainsbury-Martinez F. , Walsh C. , Cooke G. J. , Marsh D. R. 
Published: October 2024

Abstract
Interpretation of the ongoing efforts to simulate the atmospheres of potentially habitable terrestrial exoplanets requires that we understand the underlying dynamics and chemistry of such objects to a much greater degree than 1D or even simple 3D models enable. Here, for the tidally locked habitable-zone planet TRAPPIST-1e, we explore one effect which can shape the dynamics and chemistry of terrestrial planets: the inclusion of an Earth-like land–ocean distribution with orography. To do this we use the Earth-system model WACCM6/CESM2 to run a pair of TRAPPIST-1e models with N2–O2 atmospheres and with the substellar point fixed over either land or ocean. The presence of orography shapes atmospheric transport, and in the case of Earth-like orography, breaks the symmetry between the Northern and Southern Hemispheres which was previously found in slab ocean models. For example, peak zonal jet speeds in the Southern Hemisphere are 50%–100% faster than similar jets in the Northern Hemisphere. This also affects the meridional circulation, transporting equatorial material toward the south pole. As a result we also find significant changes in the atmospheric chemistry, including the accumulation of potentially lethal quantities of ozone at both the south pole and the surface. Future studies which investigate the effects of landmass distribution on the dynamics of exoplanetary atmospheres should pay close attention to both the dayside land fraction as well as the orography of the land. Simply modeling a flat landmass will not give a complete picture of its dynamical impact.
Data-driven Stellar Intrinsic Colors and Dust Reddenings for Spectrophotometric Data: From the Blue-edge Method to a Machine Learning Approach
Authors: Zhao 赵 He 赫 , Wang 王 Shu 舒 , Jiang 姜 Biwei 碧沩 , Li 李 Jun 军 , Fan 樊 Dongwei 东卫 , Ren 任 Yi 逸 , Ma 马 Xiaoxiao 晓骁 
Published: October 2024

Abstract
Intrinsic colors (ICs) of stars are essential for studies on both stellar physics and dust reddening. In this work, we developed an XGBoost model to predict ICs with the atmospheric parameters T
eff,

log

g

, and [M/H]. The model was trained and tested for three colors at Gaia and Two Micron All Sky Survey bands with 1,040,446 low-reddening sources. The atmospheric parameters were determined by the Gaia DR3 General Stellar Parameterizer from Photometry (GSP-phot) module and were validated by comparing with the Apache Point Observatory Galactic Evolution Experiment and Large Sky Area Multi-Object fiber Spectroscopic Telescope. We further confirmed that the biases in GSP-phot parameters, especially for [M/H], do not present a significant impact on the IC prediction. The generalization error of the model estimated by the test set is 0.014 mag for

(

G

BP

−

G

RP

)

0

, 0.050 mag for

(

G

BP

−

K

S

)

0

, and 0.040 mag for

(
J

−

K

S

)

0

. The model was applied to a sample containing 5,714,528 reddened stars with stellar parameters from R. Andrae et al. to calculate ICs and reddenings. The high consistency in the comparison of E(J − K
S) between our results and literature values further validates the accuracy of the XGBoost model. The variation of E(G
BP − K
S)/E(G
BP − G
RP), a representation of the extinction law, with Galactic longitude is found on large scales. This work preliminarily presents the feasibility and accuracy of the machine learning approach for IC and dust reddening calculation, whose products could be widely applied to spectrophotometric data. The data sets and trained model can be accessed via Zenodo, doi:10.5281/zenodo.12787594. Models for more bands will be completed in following work.
Tilted Disk Precession and Negative Superhumps in HS 2325+8205: A Multiwindow Analysis
Authors: Sun Qi-Bin , Qian Sheng-Bang , Zhu Li-Ying , Li Qin-Mei , Li Min-Yu , Li Ping 
Published: October 2024

Abstract
Tilted disk precession exists in different objects. Negative superhumps (NSHs) in cataclysmic variable stars are believed to arise from the interaction between the reverse precession of a tilted disk and the streams from the secondary star. Utilizing Transiting Exoplanet Survey Satellite photometry, we present a comprehensive investigation into the tilted disk precession and NSHs in the dwarf nova (DN) HS 2325+8205, employing eclipse minima, eclipse depths, NSH frequencies, and NSH amplitudes and the correlation between them as the windows. We identified NSHs with a period of 0.185671(17) day in HS 2325+8205. The NSH frequency exhibits variability with a period of 3.943(9) days, akin to the tilted disk precession period validated in nova-like stars (SDSS J0812) and intermediate polars (IPs; TV Col). The O − C of the eclipse minima were similarly found to vary cyclically in a period of 4.135(5) days, characterized by a faster rise than fall. Furthermore, the NSH amplitude exhibits complex and diverse variations, which may be linked to changes in the disk radius, the mass transfer rate, and the apparent area of the hot spot. For the first time in DNe, we observe biperiodic variations in eclipse depth (P
1 = 4.131(4) days and P
2 = 2.065(2) days ≈ P
prec/2) resembling those seen in IPs, suggesting that variations with P
2 are not attributable to an accretion curtain, as previously suspected. Moreover, NSH amplitude and eclipse depth decrease with increasing NSH frequency, while NSH amplitude correlates positively with eclipse depth. These complex variations observed across multiple observational windows provide substantial evidence for the understanding of tilted disk precession and NSHs.
Forecasting Solar Energetic Particle Events During Solar Cycles 23 and 24 Using Interpretable Machine Learning
Authors: Kasapis Spiridon , Kitiashvili Irina N. , Kosovich Paul , Kosovichev Alexander G. , Sadykov Viacheslav M. , O’Keefe Patrick , Wang Vincent 
Published: October 2024

Abstract
The prediction of solar energetic particle (SEP) events garners increasing interest as space missions extend beyond Earth’s protective magnetosphere. These events, which are, in most cases, products of magnetic-reconnection-driven processes during solar flares or fast coronal-mass-ejection-driven shock waves, pose significant radiation hazards to aviation, space-based electronics, and particularly space exploration. In this work, we utilize the recently developed data set that combines the Solar Dynamics Observatory/Space-weather Helioseismic and Magnetic Imager Active Region Patches and the Solar and Heliospheric Observatory/Space-weather Michelson Doppler Imager Active Region Patches. We employ a suite of machine learning strategies, including support vector machines (SVMs) and regression models, to evaluate the predictive potential of this new data product for a forecast of post-solar flare SEP events. Our study indicates that despite the augmented volume of data, the prediction accuracy reaches 0.7 ± 0.1 (experimental setting), which aligns with but does not exceed these published benchmarks. A linear SVM model with training and testing configurations that mimic an operational setting (positive–negative imbalance) reveals a slight increase (+0.04 ± 0.05) in the accuracy of a 14 hr SEP forecast compared to previous studies. This outcome emphasizes the imperative for more sophisticated, physics-informed models to better understand the underlying processes leading to SEP events.
Correct Criterion of Crustal Failure Driven by Intense Magnetic Stress in Neutron Stars
Authors: Kojima Yasufumi 
Published: October 2024

Abstract
Magnetar outbursts are powered by an intense magnetic field. The phenomenon has recently drawn significant attention because of a connection to some fast radio bursts that has been reported. Understanding magnetar outbursts may provide the key to mysterious transient events. The elastic deformation of the solid crust due to magnetic field evolution accumulates over a secular timescale. Eventually, the crust fractures or responds plastically beyond a particular threshold. Determination of the critical limit is required to obtain the shear strain tensor in response to magnetic stress. In some studies, the tensor was substituted with an approximate expression determined algebraically from the magnetic stress. This study evaluated the validity of the approximation by comparing it with the strain tensor obtained through appropriate calculations. The differential equations for the elastic deformation driven by the magnetic field were solved. The results indicated that the approximation did not represent the correct strain tensor value, in both magnitude and spatial profile. Previous evolutionary calculations based on spurious criteria are likely to overestimate the magnitude of the strain tensor, and crustal failure occurs on a shorter timescale. Therefore, revisiting evolutionary calculations using the correct approach is necessary. This study is essential for developing the dynamics of crustal fractures and the magnetic field evolution in a magnetar.
Giant Eruptions in Massive Stars and their Effect on the Stellar Structure
Authors: Mukhija Bhawna , Kashi Amit 
Published: October 2024

Abstract
Giant eruptions (GEs) in luminous blue variables are years-to-decades-long episodes of enhanced mass loss from the outer layers of the star during which the star undergoes major changes in its physical and observed properties. We use the Modules for Experiments in Stellar Astrophysics stellar evolution code to model the evolution of a 70 M
⊙ star that undergoes a GE. We let the star evolve to the termination of the main sequence, and when it reaches T ≃ 19,400 K we emulate a GE by removing mass from its outer layers at a rate of 0.15 M
⊙ yr−1 for 20 yr. As mass is being lost, the star contracts and releases a substantial amount of gravitational energy. The star undergoes an initial ≃3 days of expansion followed by years of contraction. During that time the star tries to reach an equilibrium state, and as a result of loss in gravitational energy, its luminosity drops about 1 order of magnitude. As the GE terminates, we let the star continue to evolve without any further mass loss and track its recovery as it regains its equilibrium by adjusting its internal structure. After ≃87 yr it reaches a state very close to the one where the GE was first initiated. We suggest that at this point another GE or a cycle of GEs may occur.
High-resolution Imaging Spectroscopy of a Tiny Sigmoidal Minifilament Eruption
Authors: Wang Jiasheng , Lee Jeongwoo , Chae Jongchul , Cao Wenda , Wang Haimin 
Published: October 2024

Abstract
Minifilament eruptions producing small jets and microflares have mostly been studied based on coronal observations at extreme-ultraviolet and X-ray wavelengths. This study presents chromospheric plasma diagnostics of a quiet-Sun minifilament of size ∼ 2″ × 5″ with a sigmoidal shape and an associated microflare observed on 2021 August 7 17:00 UT using high temporal and spatial resolution spectroscopy from the Fast Imaging Solar Spectrograph (FISS) and high-resolution magnetograms from the Near InfraRed Imaging Spectropolarimeter (NIRIS) installed on the 1.6 m Goode Solar Telescope at Big Bear Solar Observatory. Using FISS Hα and Ca ii 8542 Å line spectra at the time of the minifilament activation we determined a temperature of 8600 K and a nonthermal speed of 7.9 km s−1. During the eruption, the minifilament was no longer visible in the Ca ii 8542 Å line, and only the Hα line spectra were used to find the temperature of the minifilament, which reached 1.2 × 104 K and decreased afterward. We estimated thermal energy of 3.6 × 1024 erg from the maximum temperature and kinetic energy of 2.6 × 1024 erg from the rising speed (18 km s−1) of the minifilament. From the NIRIS magnetograms we found small-scale flux emergence and cancellation coincident with the minifilament eruption, and the magnetic energy change across the conjugate footpoints reaches 7.2 × 1025 erg. Such spectroscopic diagnostics of the chromospheric minifilament complement earlier studies of minifilament eruptions made using coronal images.
The Impact of Positive AGN Feedback on the Properties of Galaxies in a Semianalytic Model of Galaxy Formation
Authors: Contini Emanuele , Yi Sukyoung K. , Jeon Seyoung , Rhee Jinsu 
Published: October 2024

Abstract
We introduce the state-of-the-art semianalytic model Formation and Evolution of GAlaxies (FEGA), which incorporates updated prescriptions for key physical processes in galaxy formation. Notably, FEGA features an unprecedented semianalytic modeling of positive active galactic nucleus (AGN) feedback. The model combines the latest prescriptions for gas infall and cooling, a revised star formation recipe that incorporates the extended Kennicutt–Schmidt relation, disk instability, updated supernova feedback, reincorporation of ejected gas, hot gas stripping from satellite galaxies, and the formation of diffuse light. A novel description of AGN feedback is introduced, describing the positive mode as a burst of star formation from a cooling gas fraction. FEGA is rigorously calibrated using a Markov Chain Monte Carlo procedure to match the evolution of the stellar mass function from high redshift to the present. Subsequently, the model is tested against several observed and predicted scaling relations, including the star formation rate (SFR)–mass, black hole–bulge and stellar mass, stellar-to-halo mass, and red fraction–mass relations. Additionally, we test FEGA against other galaxy properties, such as the distribution of specific SFRs, stellar metallicity, and morphology. Our results demonstrate that the inclusion of positive AGN feedback can coexist with its negative counterpart without drastic alterations to other prescriptions. Importantly, this inclusion improves the ability of the model to describe the primary scaling relations observed in galaxies.
Pervasive extractivism: Petroculture and sedimented histories in Sandrine Bessora’s Petroleum
Authors: Champion Giulia 
Published: October 2024

Cet article a deux objectifs. Premièrement, il considère comment le roman de Sandrine Bessora, Petroleum (2004), utilise l’intertexte du mythe de Médée, s’inscrivant ainsi dans une tradition littéraire spécifique, pour explorer la manière dont l’histoire est écrite. Deuxièmement, il examine comment, en incorporant le mythe de Médée avec le personnage des traditions ouest-africaines de Mami Wata, le roman fictionnalise l’histoire de la colonisation comme étant connectée à celle de l’extraction, rendant ainsi visible l’insertion diffuse du pétrole aux pratiques néo-coloniales au Gabon. De cette manière, l’article montre comment l’extractivisme et le cadre théorique de la « pétroculture » permettent de réviser et de réécrire l’histoire gabonaise dans ses dimensions énergétique et coloniale. En mettant en question le déroulement traditionnel du mythe de Médée, le roman de Bessora suggère de regarder l’histoire de la colonisation et de l’extraction de ressources naturelles au Gabon à travers des perspectives pétroculturelles non-européennes.
Variedad en la unidad: la novella italiana en la construcción de El Abencerraje (II)
Authors: Resta Ilaria 
Published: October 2024

Este artículo se constituye como la segunda parte de un trabajo en torno al influjo de la novella italiana en la organización estructural y temática de El Abencerraje. Nos proponemos aquí examinar el cuento sobre la continencia de don Rodrigo, incorporado en la versión que transmite el Inventario de Villegas, poniéndolo en relación contrastiva con dos novelle, una de ser Giovanni Fiorentino y otra de Masuccio Salernitano. El propósito es el de ahondar en el posible hipotexto para el relato sobre este acontecimiento privado del caballero cristiano.
Pacto epistolar en las cartas de Jorge Guillén a Teresa: la revelación de una identidad narrativa
Authors: Saiz-Cerreda María Pilar 
Published: October 2024

A lo largo de toda su vida Jorge Guillén mantuvo, de forma constante y continua, correspondencia con numerosas personas, entre las que destacan poetas, editores, académicos y un largo etcétera. En el ámbito familiar, además de las cartas a su primera esposa, destaca el intercambio epistolar que durante décadas mantuvo con su hija Teresa. En este epistolario inédito Guillén va configurando un ethos discursivo que revelará una identidad narrativa única y singular. Pero todo ello solo es posible debido al pacto epistolar que él va a establecer y sellar con su hija. Este pacto, que tiene unas manifestaciones específicas y propias tanto a nivel pragmático, como a nivel semántico y a nivel formal, ayuda a comprender un poco mejor la profunda y rica personalidad del autor, su «esencia»; una esencia en la que están imbricados en perfecta armonía y unidad, el hombre Guillén y el poeta Guillén.
El teatro norteamericano en La estafeta literaria (1957-1962)
Authors: Espejo Romero Ramón 
Published: October 2024

El presente artículo analiza la cobertura del teatro norteamericano en La estafeta literaria entre los años 1957 y 1962, que, por una parte, se corresponden con una etapa bien definida en la evolución de esta publicación y por otro con los años de mayor apogeo del teatro estadounidense en la escena franquista. Un análisis cuantitativo de los artículos aparecidos sugiere una presencia no solo destacada sino deslindada en parte de estrenos, en línea con el perfil que se ha sugerido para La estafeta de revista cosmopolita dirigida a un lector culto. El análisis cualitativo, sin embargo, no permite confirmar tal hipótesis. Con algunos matices, lo publicado en la revista no difiere de lo que solían incluir otras publicaciones de la época y la autonomía en el análisis del fenómeno teatral deslindado de los estrenos se ha revelado ilusorio.
(Re)escribir el pasado: itinerarios de la memoria en la novela de investigación del escritor (Antonio Soler, Clara Sánchez e Ignacio Martínez de Pisón)
Authors: López López Carmen María 
Published: October 2024

Este estudio rescata el concepto de novela de investigación del escritor en El nombre que ahora digo (1999) de Antonio Soler, Lo que esconde tu nombre (2010) de Clara Sánchez y Enterrar a los muertos (2005) de Ignacio Martínez de Pisón. El hilo de Ariadna con que se tejen estas obras es el procedimiento indagatorio en el que el personaje/narrador se ve inmerso hasta modificar en un sentido radical su episteme. Conflictos bélicos como la segunda guerra mundial o la guerra civil española cristalizan en la escritura a partir del hallazgo de cuadernos, cartas, testimonios y confesiones, dando cuenta mediante la escritura del pasado de acontecimientos sangrientos, no solo a los ojos de quienes los vivieron, sino de quienes ahora los recuerdan. Frente a las claves estéticas de la novela policíaca o de la investigación del escritor que persigue la verdad de los hechos según preconiza la docuficción, este estudio se aproxima a los itinerarios de la memoria a partir de tres anclajes: investigación, comprensión y escritura, que se corresponden con las tres operaciones historiográficas distinguidas por Ricoeur para la conformación de una fenomenología de la memoria.