bluuebunny/crossref_metadata_2025_split huggingface dataset:
Are neuronal mechanisms of attention universal across human sensory and motor brain maps?
Authors: DeYoe Edgar A. , Huddleston Wendy , Greenberg Adam S. 
Published: April 2024

AbstractOne's experience of shifting attention from the color to the smell to the act of picking a flower seems like a unitary process applied, at will, to one modality after another. Yet, the unique and separable experiences of sight versus smell versus movement might suggest that the neural mechanisms of attention have been separately optimized to employ each modality to its greatest advantage. Moreover, addressing the issue of universality can be particularly difficult due to a paucity of existing cross-modal comparisons and a dearth of neurophysiological methods that can be applied equally well across disparate modalities. Here we outline some of the conceptual and methodological issues related to this problem and present an instructive example of an experimental approach that can be applied widely throughout the human brain to permit detailed, quantitative comparison of attentional mechanisms across modalities. The ultimate goal is to spur efforts across disciplines to provide a large and varied database of empirical observations that will either support the notion of a universal neural substrate for attention or more clearly identify the degree to which attentional mechanisms are specialized for each modality.
On an Application of the Hill Approach to the General Case of the Three-body Problem
Authors: Sosnitskii Stepan P. 
Published: April 2024

Abstract
In this work, we use the energy and angular momentum integrals as a resource for applying Hill’s approach to the general three-body problem. As a result, we obtain theorems on the Lagrange stability and Hill stability in the general three-body problem. Also, specific features of the general and restricted three-body problems are discussed.
The Impact of an Active Galactic Nucleus on Polycyclic Aromatic Hydrocarbon Emission in Galaxies: The Case of Ring Galaxy NGC 4138
Authors: Donnelly G. P. , Smith J. D. T. , Draine B. T. , Togi A. , Lai T. S.-Y. , Armus L. , Dale D. A. , Charmandaris V. 
Published: April 2024

Abstract
We present a focused study of radially resolved varying PAH emission in the low-luminosity active galactic nucleus (AGN)-host NGC 4138 using deep Spitzer/infrared spectrograph spectral maps. Using new model PAH spectra, we investigate whether these variations could be associated with changes to the PAH grain size distribution due to photodestruction by the AGN. Separately, we model the effects of the varying radiation field within NGC 4138, and we use this model to predict the corresponding changes in the PAH emission spectrum. We find that PAH band ratios are strongly variable with radius in this galaxy with short-to-long wavelength band ratios peaking in the starburst ring. The changing mix of starlight appears to have a considerable effect on the trends in these band ratios, and our radiation model predicts the shapes of these trends. However, the amplitude of observed variation is ∼2.5 × larger than predicted for some ratios. A cutoff of small grains in the PAH size distribution, as has been suggested for AGN, together with changes in PAH ionization fraction could explain the behavior of the shorter bands, but this model fails to reproduce longer band behaviors. Additionally, we find that short-to-long wavelength PAH band ratios increase slightly within ∼270 pc of the center, suggesting that the AGN may directly influence PAH emission there.
SN 2020udy: A New Piece of the Homogeneous Bright Group in the Diverse Iax Subclass
Authors: Singh Mridweeka , Sahu Devendra K. , Barna Barnabás , Gangopadhyay Anjasha , Dastidar Raya , Teja Rishabh Singh , Misra Kuntal , Howell D. Andrew , Wang Xiaofeng , Mo Jun , Yan Shengyu , Hiramatsu Daichi , Pellegrino Craig , Anupama G. C. , Joshi Arti , Bostroem K. Azalee , Burke Jamison , McCully Curtis , Subramanian V Rama , Li Gaici , Xi Gaobo , Li Xin , Li Zhitong , Srivastav Shubham , Im Hyobin , Dutta Anirban 
Published: April 2024

Abstract
We present optical observations and analysis of the bright type Iax supernova SN 2020udy hosted by NGC 0812. The evolution of the light curve of SN 2020udy is similar to that of other bright type Iax SNe. Analytical modeling of the quasi-bolometric light curves of SN 2020udy suggests that 0.08 ± 0.01 M
⊙ of 56Ni would have been synthesized during the explosion. The spectral features of SN 2020udy are similar to those of the bright members of type Iax class, showing a weak Si ii line. The late-time spectral sequence is mostly dominated by iron group elements with broad emission lines. Abundance tomography modeling of the spectral time series of SN 2020udy using TARDIS indicates stratification in the outer ejecta; however, to confirm this, spectral modeling at a very early phase is required. After maximum light, uniform mixing of chemical elements is sufficient to explain the spectral evolution. Unlike in the case of normal type Ia SNe, the photospheric approximation remains robust until +100 days, requiring an additional continuum source. Overall, the observational features of SN 2020udy are consistent with the deflagration of a carbon–oxygen white dwarf.
Enhanced Energy Conversion by Turbulence in Collisionless Magnetic Reconnection
Authors: Jin Runqing , Zhou Meng , Yi Yongyuan , Man Hengyan , Zhong Zhihong , Pang Ye , Deng Xiaohua 
Published: April 2024

Abstract
Magnetic reconnection and turbulence are two of the most significant mechanisms for energy dissipation in collisionless plasma. The role of turbulence in magnetic reconnection poses an outstanding problem in astrophysics and plasma physics. It is still unclear whether turbulence can modify the reconnection process by enhancing the reconnection rate or energy conversion rate. In this study, utilizing unprecedented high-resolution data obtained from the Magnetospheric Multiscale spacecraft, we provide direct evidence that turbulence plays a vital role in promoting energy conversion during reconnection. We reached this conclusion by comparing magnetotail reconnection events with similar inflow Alfvén speed and plasma β but varying amplitudes of turbulence. The disparity in energy conversion was attributed to the strength of turbulence. Stronger turbulence generates more coherent structures with smaller spatial scales, which are pivotal contributors to energy conversion during reconnection. However, we find that turbulence has negligible impact on particle heating, but it does affect the ion bulk kinetic energy in these two events. These findings significantly advance our understanding of the relationship between turbulence and reconnection in astrophysical plasmas.
[N i] 10400/10410 Å Lines as Possible Disk Wind Tracers in a Young Intermediate-mass Star
Authors: Katoh Haruki , Yasui Chikako , Ikeda Yuji , Kobayashi Naoto , Matsunaga Noriyuki , Kondo Sohei , Sameshima Hiroaki , Hamano Satoshi , Mizumoto Misaki , Kawakita Hideyo , Fukue Kei , Otsubo Shogo , Takenaka Keiichi 
Published: April 2024

Abstract
In this study, we performed high-resolution near-infrared (NIR) spectroscopy (R = 28,000; λ = 0.90–1.35 μm) with a high signal-to-noise ratio on HD 200775, a very young (∼0.1 Myr old) and massive intermediate-mass star (a binary star with a mass of about 10 M
⊙ each) with a protoplanetary disk. The obtained spectra show eight forbidden lines of three elements: two of [S ii] (10289 and 10323 Å), two of [N i] (10400 and 10410 Å), and four of [Fe ii] (12570, 12946, 12981, and 13209 Å). This is the first time that the [N i] lines are detected in a young stellar object with a doublet deblended. Gaussian fitting of the spectra indicates that all line profiles have low-velocity components and exhibit blueshifted features, suggesting that all lines originate from the disk winds (magnetohydrodynamic disk wind and/or photoevaporative wind). Based on the fit, the [N i] and [Fe ii] lines are categorized into narrow components, while the [S ii] lines are at the boundary between broad and narrow components. These forbidden lines are suggested to be very promising disk wind tracers among the existing ones because they are in the NIR-wavelength range, which can be observed from early stages with high sensitivities. Among these lines, [N i] lines would be a rather powerful probe for deriving the basic physical parameters of disk wind gases. However, the study of these lines herein is limited to one object; thus, further studies are needed to examine their properties.
Distribution Properties of the 6.7 GHz Methanol Masers and Their Surrounding Gases in the Milky Way
Authors: Yang Tian , Chen Xi , Zhang Yan-Kun , Ouyang Xu-Jia , Song Shi-Min , Chen Jia-Liang , Lu Ying 
Published: April 2024

Abstract
An updated catalog consisting of 1092 6.7 GHz methanol maser sources is reported in this work. Additionally, the NH3 (1, 1), NH3 (2, 2), and NH3 (3, 3) transitions were observed toward 214 star-forming regions using the Shanghai Tianma radio telescope in order to examine the differences in physical environments, such as the excitation temperature and column density of molecular clouds associated with methanol masers on the Galactic scale. Statistical results reveal that the number of 6.7 GHz methanol masers in the Perseus arm is significantly lower than that in the other three main spiral arms. In addition, the Perseus arm also has the lowest gas column density among the main spiral arms traced by the NH3 observations. Both findings suggest that the Perseus arm has the lowest rate of high-mass star formation compared to the other three main spiral arms. We also observed a trend in which both the luminosity of the 6.7 GHz methanol masers and the ammonia gas column density decreased with the galactocentric distance. This finding indicates that the density of material in the inner Milky Way is generally higher than that in the outer Milky Way. This further suggests that high-mass stars are more easily formed at the head of the spiral arms. Furthermore, we found that the column density of ammonia gas is higher in the regions on the arms than in the inter-arm regions, supporting that the former is more likely to be the birthplace of high-mass stars.
Toward More Accurate Synthetic Reflection Spectra: Improving the Calculations of Returning Radiation
Authors: Mirzaev Temurbek , Riaz Shafqat , Abdikamalov Askar B. , Bambi Cosimo , Dauser Thomas , Garcia Javier A. , Jiang Jiachen , Liu Honghui , Shashank Swarnim 
Published: April 2024

Abstract
We present a new model to calculate reflection spectra of thin accretion disks in Kerr spacetimes. Our model includes the effect of returning radiation, which is the radiation that is emitted by the disk and returns to the disk because of the strong light bending near a black hole. The major improvement with respect to the existing models is that it calculates the reflection spectrum at every point on the disk by using the actual spectrum of the incident radiation. Assuming a lamppost coronal geometry, we simulate simultaneous observations of NICER and NuSTAR of bright Galactic black holes and we fit the simulated data with the latest version of relxill (modified to read the table of reflionx, which is the nonrelativistic reflection model used in our calculations). We find that relxill with returning radiation cannot fit well the simulated data when the black hole spin parameter is very high and the coronal height and disk’s ionization parameter are low, and some parameters can be significantly overestimated or underestimated. We can find better fits and recover the correct input parameters as the value of the black hole spin parameter decreases and the value of the coronal height increases.
Identifying Plasma Fractionation Processes in the Chromosphere Using IRIS
Authors: Long David M. , Baker Deborah , To Andy S. H. , van Driel-Gesztelyi Lidia , Brooks David H. , Stangalini Marco , Murabito Mariarita , James Alexander W. , Mathioudakis Mihalis , Testa Paola 
Published: April 2024

Abstract
The composition of the solar corona differs from that of the photosphere, with the plasma thought to fractionate in the solar chromosphere according to the first ionization potential (FIP) of the different elements. This produces a FIP bias, wherein elements with a low FIP are preferentially enhanced in the corona compared to their photospheric abundance, but direct observations of this process remain elusive. Here, we use a series of spectroscopic observations of active region AR 12759 as it transited the solar disk over a period of 6 days from 2020 April 2–7 taken using the Hinode Extreme ultraviolet Imaging Spectrometer and Interface Region Imaging Spectrograph (IRIS) instruments to look for signatures of plasma fractionation in the solar chromosphere. Using the Si x/S x and Ca xiv/Ar xiv diagnostics, we find distinct differences between the FIP bias of the leading and following polarities of the active region. The widths of the IRIS Si iv lines exhibited clear differences between the leading and following polarity regions, indicating increased unresolved wave activity in the following polarity region compared to the leading polarity region, with the chromospheric velocities derived using the Mg ii lines exhibiting comparable, albeit much weaker, behavior. These results are consistent with plasma fractionation via resonant/nonresonant waves at different locations in the solar chromosphere following the ponderomotive force model, and indicate that IRIS could be used to further study this fundamental physical process.
Visit Nearby Halo Substructures Using LAMOST DR9 MRS Data
Authors: Tang 唐 Xin-Zhe 馨哲 , Zhao 赵 Jing-Kun 景昆 , Yang 杨 Yong 勇 , Ye 叶 Xian-Hao 先豪 , Zhao 赵 Gang 刚 , Gao 高 Qi 启 
Published: April 2024

Abstract
Based on the LAMOST DR9 Medium Resolution Spectra (MRS) catalog, combined with astrometries from Gaia DR3, we conducted an investigation into the substructures in the stellar halo to obtain their chemical and kinematic information. We employed the HDBSCAN algorithm in the (L

z
, E, L

xy
) space for clustering and utilized Mahalanobis distance to merge the clustering results. Ultimately, within the LAMOST DR9 MRS catalog, we identified members of Gaia–Sausage–Enceladus (GSE), Helmi streams, and the high-α disk and in situ halo. Additionally, there are three clusters that cannot be correlated with known substructures. Based on their angular momentum (L

z
) characteristics, we have tentatively named two of them High-L

z
-Cluster-1 (HLC-1) and High-L

z
-Cluster-2 (HLC-2), both exhibiting high angular momentum (L

z
) features. The third cluster, owing to its extremely low L

z
, is termed the Low-L

z
-Cluster. Then detailed analysis about those substructures are executed including member stars’ identification and kinematic and chemical distribution. The resulting GSE member stars exhibit a well-defined metallicity distribution function with its peak at [Fe/H] ∼ −1.2, consistent with previous findings, and we found there appear to be some differences in the distribution on the V
total–r
gal plane between GSE and its included Splash component. Regarding Helmi streams, in the [Mg/Fe]–[Fe/H] plane we detected potential traces of the α-knee phenomenon at [Fe/H] ∼ −1.53. Finally, we tentatively provide the possible origin for the HLC-1 and HLC-2.
Parallel Diffusion Coefficient of Energetic Charged Particles in the Inner Heliosphere from the Turbulent Magnetic Fields Measured by Parker Solar Probe
Authors: Chen Xiaohang , Giacalone Joe , Guo Fan , Klein Kristopher G. 
Published: April 2024

Abstract
Diffusion coefficients of energetic charged particles in turbulent magnetic fields are a fundamental aspect of diffusive transport theory but remain incompletely understood. In this work, we use quasi-linear theory to evaluate the spatial variation of the parallel diffusion coefficient κ
∥ from the measured magnetic turbulence power spectra in the inner heliosphere. We consider the magnetic field and plasma velocity measurements from Parker Solar Probe made during Orbits 5–13. The parallel diffusion coefficient is calculated as a function of radial distance from 0.062 to 0.8 au, and the particle energy from 100 keV to 1 GeV. We find that κ
∥ increases exponentially with both heliocentric distance and energy of particles. The fluctuations in κ
∥ are related to the episodes of large-scale magnetic structures in the solar wind. By fitting the results, we also provide an empirical formula of κ
∥ = (5.16 ± 1.22) × 1018
r
1.17±0.08
E
0.71±0.02 (cm2 s−1) in the inner heliosphere, which can be used as a reference in studying the transport and acceleration of solar energetic particles as well as the modulation of cosmic rays.
Suppression of Star Formation in Galaxy Pairs
Authors: Feng 冯 Shuai 帅 , Shen 沈 Shi-Yin 世银 , Yuan 袁 Fang-Ting 方婷 , Zhong 钟 Wen-Xin 文心 , Cui 崔 Wen-Yuan 文元 , Li 李 Lin-Lin 林林 
Published: April 2024

Abstract
We investigate the suppression of star formation in galaxy pairs based on the isolated galaxy pair sample derived from the Sloan Digital Sky Survey survey. By comparing the star formation rate between late-type galaxies (LTGs) in galaxy pairs and those in the isolated environment, we detect a signal of the suppression of star formation in galaxy pairs at d
p < 100 kpc and 200 kpc < d
p < 350 kpc. The occurrence of the suppression of star formation in these LTGs requires their companion galaxies to have an early-type morphology (n

s
> 2.5). The suppression of star formation in wide galaxy pairs at 200 kpc < d
p < 350 kpc mainly occurs in massive LTGs, while in close galaxy pairs at d
p < 100 kpc, it only appears in LTGs with a massive companion (

log

M

⋆

>
11.0

), nearly independent of their own stellar mass. Based on these findings, we infer that the suppression of star formation in wide galaxy pairs is actually a result of galaxy conformity, while in close galaxy pairs, it stems from the influence of hot circumgalactic medium surrounding companion galaxies.
Study of Magnetic Field and Turbulence in the TeV Halo around the Monogem Pulsar
Authors: Malik Sunil , Yuen Ka Ho , Yan Huirong 
Published: April 2024

Abstract
Magnetic fields are ubiquitous in the interstellar medium, including extended objects such as supernova remnants and diffuse halos around pulsars. Its turbulent characteristics govern the diffusion of cosmic rays and the multiwavelength emission from pulsar wind nebulae (PWNe). However, the geometry and turbulence nature of the magnetic fields in the ambient region of PWN is still unknown. Recent gamma-ray observations from HAWC and synchrotron observations suggest a highly suppressed diffusion coefficient compared to the mean interstellar value. In this study, we present the first direct observational evidence of the orientation of the mean magnetic field and turbulent characteristics by employing a recently developed statistical parameter “Y
turb” in the extended halo around the Monogem pulsar. Our study points to two possible scenarios: nearly aligned toward the line of sight (LOS) with compressible modes dominance or high inclination angle toward the LOS and characterized by Alfvénic turbulence. The first scenario appears consistent with other observational signatures. Furthermore, we report that the magnetic field has an observed correlation length of approximately 3 ± 0.6 pc in the Monogem halo. Our study highlights the pivotal role of magnetic field and turbulence in unraveling the physical processes in TeV halos and cosmic-ray transport.
Mini-RF S-band Radar Characterization of a Lunar South Pole–crossing Tycho Ray: Implications for Sampling Strategies
Authors: Rivera-Valentín Edgard G. , Fassett Caleb I. , Denevi Brett W. , Meyer Heather M. , Neish Catherine D. , Morgan Gareth A. , Cahill Joshua T. S. , Stickle Angela M. , Patterson G. Wesley 
Published: April 2024

Abstract
One of the youngest features on the Moon is Tycho, an 85 km diameter impact crater with a vast ray system that spans much of the lunar nearside. As such, it serves as an important stratigraphic marker for the Moon. One of Tycho’s longest rays crosses the South Pole, where it intersects several candidate landing sites for NASA’s Artemis III mission, which intends to return new lunar samples. Identification of ray-related effects are thus important to understand the provenance of collected material. To help contextualize sampling strategies, here we characterize the South Pole–crossing Tycho ray using monostatic S-band radar observations from the Lunar Reconnaissance Orbiter’s Miniature Radio Frequency instrument. We found that the ray is a ∼15 km wide radar-bright feature extending at least ∼1600 km from Tycho. Polarimetric analysis revealed that the measured radar backscatter is consistent with a terrain enhanced in centimeter-to-decimeter-scale scatterers. Moreover, we found that the abundance of these scatterers likely decreases with distance from the primary crater, suggesting there may be less Tycho-disturbed material, in particular, poleward of 85°S, where the candidate landing sites are located. Nevertheless, we identified craters along the ray and, importantly, within the Haworth candidate landing site that exhibit secondary crater characteristics, such as radar-bright, asymmetric ejecta deposits. We showed, based on solar illumination and topographic slopes, that the likely Tycho-related secondaries within Haworth are accessible by landed missions. Exploration of this site may thus directly sample Tycho-disturbed material, including a nearby permanently shadowed region, providing new insights into lunar surface processes.
L’enseignement du droit économique et la transition écologique
Authors: Teller Marina 
Published: April 2024

Cette contribution a pour objectif de faire un retour d’expérience sur l’enseignement du droit économique au regard de la transition écologique, après plus d’une décennie d’enseignement de cette discipline au sein de l’Université Côte d’Azur. Quelle est la place de la transition écologique au sein du droit économique ? Plus spécifiquement, ce droit permet-il une meilleure appréhension des enjeux environnementaux que ne le font les autres branches du droit ? Afin de démontrer la pertinence et l’originalité de la méthode du droit économique pour faire face aux défis de la transition écologique, il convient dans un premier temps de rappeler les postulats fondamentaux de cette école de pensée. Il en ressort que seule une méthode substantielle permet de répondre aux enjeux véritablement globaux que soulève cette transition.
La transition écologique et l’enseignement de nouvelles disciplines juridiques écologico-économiques
Authors: Couveinhes Matsumoto Florian 
Published: April 2024

Le sujet de la transition écologique remet en cause les catégories disciplinaires établies. Dans le domaine du droit, c’est particulièrement le cas de la division entre droit de l’environnement et droit économique, ou entre le premier et les différentes branches du second. Du point de vue de l’enseignement, répondre à cette remise en cause impose d’élaborer des cours et manuels nouveaux, dépassant le dogme du « soutien mutuel » et faisant face au problème fondamental qui est que les règles du droit économique sont susceptibles d’empêcher le droit de l’environnement d’atteindre ses objectifs, et vice-versa.