bluuebunny/crossref_metadata_2025_split huggingface dataset:
AU Microscopii in the Far-UV: Observations in Quiescence, during Flares, and Implications for AU Mic b and c
Authors: Feinstein Adina D. , France Kevin , Youngblood Allison , Duvvuri Girish M. , Teal D. J. , Cauley P. Wilson , Seligman Darryl Z. , Gaidos Eric , Kempton Eliza M.-R. , Bean Jacob L. , Diamond-Lowe Hannah , Newton Elisabeth , Ginzburg Sivan , Plavchan Peter , Gao Peter , Schlichting Hilke 
Published: August 2022

Abstract
High-energy X-ray and ultraviolet (UV) radiation from young stars impacts planetary atmospheric chemistry and mass loss. The active ∼22 Myr M dwarf AU Mic hosts two exoplanets orbiting interior to its debris disk. Therefore, this system provides a unique opportunity to quantify the effects of stellar X-ray and UV irradiation on planetary atmospheres as a function of both age and orbital separation. In this paper, we present over 5 hr of far-UV (FUV) observations of AU Mic taken with the Cosmic Origins Spectrograph (COS; 1070-1360 Å) on the Hubble Space Telescope (HST). We provide an itemization of 120 emission features in the HST/COS FUV spectrum and quantify the flux contributions from formation temperatures ranging from 104 to 107 K. We detect 13 flares in the FUV white-light curve with energies ranging from 1029 to 1031 erg s. The majority of the energy in each of these flares is released from the transition region between the chromosphere and the corona. There is a 100× increase in flux at continuum wavelengths λ < 1100 Å in each flare, which may be caused by thermal Bremsstrahlung emission. We calculate that the baseline atmospheric mass-loss rate for AU Mic b is ∼108 g s−1, although this rate can be as high as ∼1014 g s−1 during flares with

L

flare

≃

10

33

erg s−1. Finally, we model the transmission spectra for AU Mic b and c with a new panchromatic spectrum of AU Mic and motivate future JWST observations of these planets.
A Comprehensive Perturbative Formalism for Phase Mixing in Perturbed Disks. I. Phase Spirals in an Infinite, Isothermal Slab
Authors: Banik Uddipan , Weinberg Martin D. , van den Bosch Frank C. 
Published: August 2022

Abstract
Galactic disks are highly responsive systems that often undergo external perturbations and subsequent collisionless equilibration, predominantly via phase mixing. We use linear perturbation theory to study the response of infinite isothermal slab analogs of disks to perturbations with diverse spatiotemporal characteristics. Without self-gravity of the response, the dominant Fourier modes that get excited in a disk are the bending and breathing modes, which, due to vertical phase mixing, trigger local phase-space spirals that are one- and two-armed, respectively. We demonstrate how the lateral streaming motion of slab stars causes phase spirals to damp out over time. The ratio of the perturbation timescale (τ
P) to the local, vertical oscillation time (τ

z
) ultimately decides which of the two modes is excited. Faster, more impulsive (τ
P < τ

z
) and slower, more adiabatic (τ
P > τ

z
) perturbations excite stronger breathing and bending modes, respectively, although the response to very slow perturbations is exponentially suppressed. For encounters with satellite galaxies, this translates to more distant and more perpendicular encounters triggering stronger bending modes. We compute the direct response of the Milky Way disk to several of its satellite galaxies and find that recent encounters with all of them excite bending modes in the solar neighborhood. The encounter with Sagittarius triggers a response that is at least 1–2 orders of magnitude larger than that due to any other satellite, including the Large Magellanic Cloud. We briefly discuss how ignoring the presence of a dark matter halo and the self-gravity of the response might impact our conclusions.
Ice Age: Chemodynamical Modeling of Cha-MMS1 to Predict New Solid-phase Species for Detection with JWST
Authors: Jin Miwha , Lam Ka Ho , McClure Melissa K. , van Scheltinga Jeroen Terwisscha , Li Zhi-Yun , Boogert Adwin , Herbst Eric , Davis Shane W. , Garrod Robin T. 
Published: August 2022

Abstract
Chemical models and experiments indicate that interstellar dust grains and their ice mantles play an important role in the production of complex organic molecules (COMs). To date, the most complex solid-phase molecule detected with certainty in the interstellar medium is methanol, but the James Webb Space Telescope (JWST) may be able to identify still larger organic species. In this study, we use a coupled chemodynamical model to predict new candidate species for JWST detection toward the young star-forming core Cha-MMS1, combining the gas–grain chemical kinetic code MAGICKAL with a 1D radiative hydrodynamics simulation using Athena++. With this model, the relative abundances of the main ice constituents with respect to water toward the core center match well with typical observational values, providing a firm basis to explore the ice chemistry. Six oxygen-bearing COMs (ethanol, dimethyl ether, acetaldehyde, methyl formate, methoxy methanol, and acetic acid), as well as formic acid, show abundances as high as, or exceeding, 0.01% with respect to water ice. Based on the modeled ice composition, the infrared spectrum is synthesized to diagnose the detectability of the new ice species. The contribution of COMs to IR absorption bands is minor compared to the main ice constituents, and the identification of COM ice toward the core center of Cha-MMS1 with the JWST NIRCAM/Wide Field Slitless Spectroscopy (2.4–5.0 μm) may be unlikely. However, MIRI observations (5–28 μm) toward COM-rich environments where solid-phase COM abundances exceed 1% with respect to the column density of water ice might reveal the distinctive ice features of COMs.
The Active Galactic Nuclei in the Hobby–Eberly Telescope Dark Energy Experiment Survey (HETDEX). II. Luminosity Function
Authors: Liu Chenxu , Gebhardt Karl , Cooper Erin Mentuch , Zhang Yechi , Schneider Donald P. , Ciardullo Robin , Davis Dustin , Farrow Daniel J. , Finkelstein Steven L. , Gronwall Caryl , Hill Gary J. , House Lindsay , Jeong Donghui , Kollatschny Wolfram , Niemeyer Maja Lujan , Tuttle Sarah ,   (The HETDEX Collaboration)
Published: August 2022

Abstract
We present the Lyα emission line luminosity function (LF) of the active galactic nuclei (AGN) in the first release of the Hobby–Eberly Telescope Dark Energy Experiment Survey (HETDEX) AGN catalog. The AGN are selected either by emission line pairs characteristic of AGN or by a single broad emission line, free of any photometric preselections (magnitude/color/morphology). The sample consists of 2346 AGN spanning 1.88 < z < 3.53, covering an effective area of 30.61 deg2. Approximately 2.6% of the HETDEX AGN are not detected at >5σ confidence at r ∼ 26 in the deepest r-band images we have searched. The Lyα line luminosity ranges from ∼1042.3 to 1045.9 erg s−1. Our Lyα LF shows a turnover luminosity with opposite slopes on the bright end and the faint end: The space density is highest at

L

Ly
α

∗

=

10
43.4

erg s−1. We explore the evolution of the AGN LF over a broader redshift range (0.8 < z < 3); constructing the rest-frame ultraviolet (UV) LF with the 1450 Å monochromatic luminosity of the power-law component of the continuum (M1450) from M
1450 ∼ −18 to −27.5. We divide the sample into three redshift bins (z ∼ 1.5, 2.1, and 2.6). In all three redshift bins, our UV LFs indicate that the space density of AGN is highest at the turnover luminosity

M

1450

*

with opposite slopes on the bright end and the faint end. The M
1450 LFs in the three redshift bins can be well fit with a luminosity evolution and density evolution model: the turnover luminosity (

M

1450

*

) increases, and the turnover density (Φ*) decreases with increasing redshift.
The Effects of Radiative Feedback and Supernova-induced Turbulence on Early Galaxies
Authors: Sarmento Richard , Scannapieco Evan 
Published: August 2022

Abstract
The recently launched James Webb Space Telescope promises unparalleled advances in our understanding of the first stars and galaxies, but realizing this potential requires cosmological simulations that capture the key physical processes that affected these objects. Here, we show that radiative transfer and subgrid turbulent mixing are two such processes. By comparing simulations with and without radiative transfer but with exactly the same physical parameters and subgrid turbulent mixing model, we show that tracking radiative transfer suppresses the Population III star formation density by a factor ≈4. In both simulations, ≳90% of Population III stars are found in the unresolved pristine regions tracked by our subgrid model, which does a better job at modeling the regions surrounding proto-galaxy cores where metals from supernovae take tens of megayears to mix thoroughly. At the same time, radiative transfer suppresses Population III star formation, via the development of ionized bubbles that slow gas accretion in these regions, and it results in compact high-redshift galaxies that are surrounded by isolated low-mass satellites. Thus, turbulent mixing and radiative transfer are both essential processes that must be included to accurately model the morphology, composition, and growth of primordial galaxies.
Black Hole–Black Hole Total Merger Mass and the Origin of LIGO/Virgo Sources
Authors: Belczynski Krzysztof , Doctor Zoheyr , Zevin Michael , Olejak Aleksandra , Banerje Sambaran , Chattopadhyay Debatri 
Published: August 2022

Abstract
The LIGO–Virgo–KAGRA (LVK) Collaboration has reported nearly 100 black hole (BH)–BH mergers. LVK provides estimates of rates, masses, effective spins, and redshifts for these mergers. Yet the formation channel(s) of the mergers remains uncertain. One way to search for a formation site is to contrast the properties of detected BH–BH mergers with different models of BH–BH merger formation. Our study is designed to investigate the usefulness of the total BH–BH merger mass and its evolution with redshift in establishing the origin of gravitational-wave sources. We find that the average intrinsic BH–BH total merger mass shows exceptionally different behaviors for the models that we adopt for our analysis. In the local universe (z = 0), the average merger mass changes from

M

¯

tot
,
int

∼
25

M

⊙

for the common envelope binary evolution and open cluster formation channels, to

M

¯

tot
,
int

∼
30

M

⊙

for the stable Roche lobe overflow binary channel, to

M

¯

tot
,
int

∼
45

M

⊙

for the globular cluster channel. These differences are even more pronounced at larger redshifts. However, these differences are diminished when considering the LVK O3 detector sensitivity. A comparison with the LVK O3 data shows that none of our adopted models can match the data, despite the large errors on BH–BH masses and redshifts. We emphasize that our conclusions are derived from a small set of six models that are subject to numerous known uncertainties. We also note that BH–BH mergers may originate from a mix of several channels, and that other (than those adopted here) BH–BH formation channels may exist.
The Spectral Energy Distributions for 4FGL Blazars
Authors: Yang J. H. , Fan J. H. , Liu Y. , Tuo M. X. , Pei Z. Y. , Yang W. X. , Yuan Y. H. , He S. L. , Wang S. H. , Wang X. C. , Chen X. J. , Qu X. H. , Cao Q. , Tao Q. Y. , Zhang Y. L. , Liu C. Q. , Nie J. J. , Liu L. F. , Jiang D. K. , Jiang A. N. , Liu B. , Yang R. S. 
Published: August 2022

Abstract
In this paper, the multiwavelength data from radio to X-ray bands for 2709 blazars in the 4FGL-DR3 catalog are compiled to calculate their spectral energy distributions using a parabolic equation

log
(
ν

f

ν

)
=

P

1

log
ν
−

P

2

2

+

P

3

. Some important parameters including spectral curvature (P
1), synchrotron peak frequency (P
2,

log

ν

p

), and peak luminosity (

log

L

p

) are obtained. Based on those parameters, we discussed the classification of blazars using the “Bayesian classification” and investigated some mutual correlations. We came to the following results. (1) Based on the Bayesian classification of synchrotron peak frequencies, the 2709 blazars can be classified into three subclasses, i.e.,

log
(

ν

p

/

Hz
)
<
13.7

for low synchrotron peak blazars (LSPs),

13.7
<
log
(

ν

p

/

Hz
)
<
14.9

for intermediate synchrotron peak blazars (ISPs), and

log
(

ν

p

/

Hz
)
>
14.9

for high synchrotron peak blazars (HSPs), and there are 820 HSPs, 750 ISPs, and 1139 LSPs. (2) The γ-ray emission has the closest relationship with radio emission, followed by optical emission, while the weakest relationship is that with X-ray emission. The γ-ray luminosity is also correlated with the synchrotron peak luminosity. (3) There are strong positive correlations between the curvature (1/∣P
1∣) and the peak frequency (

log

ν

p

) for all subclasses (FSRQs, (high, intermediate, and low) BL Lacertae objects). For different subclasses, the correlation slopes are different, which implies that there are different acceleration mechanisms and emission processes for different subclasses of blazars.
The Fossil Lithistida Collection at the Natural History Museum, London (UK)
Authors: Sendino Consuelo , Tucker Andrew 
Published: August 2022

This paper presents a quantitative and detailed description of the Fossil Lithistida Collection in the Natural History Museum, London. This collection started to be built with the first fossil sponges from the Cretaceous of Wiltshire, collected by William Smith in 1816 and 1818 for the first geological map of England. The latest specimen to enter the collection was collected from the Permo-Carboniferous of Norway by Angela Milner, a researcher at the Museum, in 2000. Although they are mostly from the Cretaceous of England, lithistids are represented from the Cambrian to Cenozoic of England. This makes this collection key for studying this group. Lithistid study will help with understanding of biosilicification evolution in sponges to unlock the changing patterns in the silica cycle in the oceans through geological time.
A dataset with information about all the Fossil Lithistida Collection is available through the NHM Data Portal and Suppl. material 1. This dataset includes taxonomic identifications, registration numbers of the specimens, geographic and stratigraphic details, information about specimen collectors and donors, type status and publications where the specimens have been referred.
Proposal (30) to conserve the name Polysticho setiferi-Fraxinetum excelsioris (Tüxen et Oberdorfer 1958) Rivas-Martínez ex Díaz et Fernández Prieto 1994 with a conserved type
Authors: Loidi Javier , Amigo Javier , Bueno Álvaro , Herrera Mercedes , Rodríguez-Guitián Manuel A. 
Published: August 2022

Abstract: The association Polysticho setiferi-Fraxinetum excelsioris was described as a meso-eutrophic thermophilic forest dominated by common oak (Quercus robur) with a distribution that includes the Oviedo district in Asturias and the Basque-Cantabrian area (N Spain and SW France). However, when a lectotype was chosen to comply with Article 19 of the ICPN, a relevé dominated by beech was selected, which leads to interpretive problems. Given that the most widespread interpretation of this association in the phytosociological literature is the one established by its original authors (i.e., a meso-eutrophic oak-ash forest), we consider that this name should be retained, but its type should be changed to a conserved neotypus according to Article 53 of the 4th edition of the ICPN.
(30) Polysticho setiferi-Fraxinetum excelsioris (Tüxen et Oberdorfer 1958) Rivas-Martínez ex Díaz et Fernández Prieto 1994
Typus: see below (typus cons. propos.)
Taxonomic reference: Castroviejo et al. (1986–2021).
Syntaxonomic reference: Rivas-Martínez (2011).
Abbreviations: ICPN = International Code of Phytosociological Nomenclature.
Le bore-out ou l’épuisement professionnel par l’ennui : un corolaire à la souffrance au travail
Authors: Chtioui Aziz , Hechiche Salah Lamia , Ben Othmane Sandra 
Published: August 2022

Le travail occupe de nos jours une place importante dans la vie des individus. Il constitue un moyen privilégié pour se réaliser et s’insérer dans la société. Cependant, au cours de ces dernières décennies, le travail a subi d’importantes mutations affectant l’environnement du travail. La digitalisation, l'automatisation du travail, la précarité de l'emploi et les périodes de restructuration ont ainsi bouleversé le rapport de l’individu avec son travail. Si certains employés semblent surchargés jusqu’à l’épuisement, d'autres, à l'opposé, semblent mourir d'ennui au travail. Se retrouver dans une situation d'ennui mortel au travail peut conduire les employés à l’épuisement professionnel ou bore-out. Or, le bore-out peut générer des conséquences néfastes et constituer une source de souffrance pour les employés concernés. En effet, la souffrance au travail survient lorsque l’employé se heurte à des expériences psychologiques insurmontables et déstabilisantes. De nombreux auteurs associent le concept de « bore-out » à celui de « souffrance au travail », sans pour autant énoncer explicitement la manière dont ils sont associés ; d'où l'intérêt de comprendre en profondeur la relation entre ces deux concepts. Pour ce faire, des entretiens en profondeur auprès de 22 employés appartenant à des fonctions différentes nous ont permis de constater que la situation de bore-out vécue par nos informants génère de nombreux sentiments (inutilité, honte, tristesse, frustration et stagnation mentale) à l’origine d’une grande souffrance au travail
1783, la fin du ciel ancien
Authors: Vasak Anouchka 
Published: August 2022

1783 : c’est l’année des premières expériences aérostatiques, celles des frères Montgolfier et de Pilâtre de Rozier. Mais 1783 voit d’autres événements dans le ciel. Le plus connu est celui de l’éruption du volcan Laki en Islande avec ses conséquences météorologiques et leurs effets désastreux sur les récoltes, sans que le lien soit alors établi entre ces phénomènes. 1783 est aussi l’année où Lavoisier publie ses Réflexions sur le phlogistique qui mettent fin à la théorie des quatre éléments. La perspective simultanéiste, à partir d’un plan en coupe de l’année 1783, permet de considérer le ciel comme le lieu de nouvelles expériences, mais aussi comme le laboratoire d’une vision du monde inédite, sinon globale, du moins plus universelle. Il s’y joue, à quelques années du début de la Révolution, la fin des théories antiques, notamment aristotéliciennes, et l’entrée dans un monde chaotique, mais « connecté ».
A formação de professores alfabetizadores na escola pública: uma análise crítica
Authors: De Brito Lúcia Helena , Vicente da Silva Sirneto 
Published: August 2022

Este artigo objetiva analisar o modelo de formação docente ofertado pelos programas de erradicação do analfabetismo infantil PAIC e PNAIC, com foco na experiência de sua implementação no município de Russas-CE. Para tanto, toma como método de análise o materialismo histórico-dialético, apoiando-se em uma pesquisa bibliográfica fundamentada com relevo em Marx, Saviani, Alves, Shiroma et al., Giroux, Duarte, dentre outros; na análise dos documentos oficiais que definem as diretrizes para a formação dos docentes desses programas; e em pesquisa de campo. Os resultados permitem concluir que os testes padronizados condicionam o modelo de formação docente; ocasionam o estreitamento curricular; impedem em larga medida a autonomia pedagógica dos professores, que não se reconhecem na prática que desenvolvem; impõem uma rotina pedagógica e o uso de material estruturado nas aulas, elaborado por empresas, as quais desconsideram a totalidade na qual a escola, alunos e professores estão inseridos.
Palavras-chave: Políticas Públicas Educacionais; Gestão por Resultados; Formação de Professores Alfabetizadores.
Influence of Transaction Cost Determinants on Credit Customer Category of Commercial Banks in Tanzania
Authors: Nguvava Heriel Emanuel 
Published: August 2022

The provision of credit services in rural areas is a challenge as agriculture and other rural economic activities have unique characteristics of dependence on natural resources, long production cycles and vulnerability to multiple risks. This paper aims to analyse transaction cost as the determinants of the choice of credit customer category for commercial bank’s credit business scale-up in Tanzania. Primary data for this study were collected from 37 registered and licensed commercial banks in January 2018 through structured questionnaires. The main sources of secondary data were peer-reviewed journal articles on transaction cost economics and rural financing. Data were analysed quantitatively through the logistic regression method. Key findings revealed that commercial banks have failed to scale up their credit operations to rural-based customers due to high transaction costs. This fact emanated from commercial banks’ preference of transacting credits directly with individual borrowers instead of using intermediaries, thus multiplying transaction costs, especially when dealing with rural-based borrowers. Therefore, commercial banks believe to be better off with few urban-based credit customers. This study recommended that commercial banks should use multiple credit governance structures (CGSs)\ (methods for credits delivery) to mitigate transaction costs when giving credits. Direct channels should be opted for when dealing with urban-based borrowers since low transaction costs are involved. Indirect channels with intermediaries should be opted for when scaling-up credit operations to rural-based borrowers since they allow the spreading of credit transaction costs throughout the credit supply channel.
Effects of Government Debt on Monetary Policy Strategy in Tanzania
Authors: Mwankemwa Suma Philbert 
Published: August 2022

This paper examines the fiscal dominance hypothesis in Tanzania by exploring the relationship between the monetary base and the government debt using monthly data from 2003:1 to 2019:12. Results from formal statistical tests indicate no evidence of a long-run relationship between the variables. Structural vector autoregressive model is thus estimated to analyse the short-run dynamics. The findings point to a positive and statistically significant impact of government debt on monetary base. The findings identifies political phenomenon that before the fourth phase government (2003-2005), monetary policy witnessed relatively intensive fiscal dominance as compared to the fourth phase (2005-2015) and fifth phase government (2015-2019). However, in comparison with the fourth phase government, findings suggest that during the first four years of the fifth phase government, monetary policy encountered a relatively high fiscal influence, partly attributed to implementation of huge development projects and reduction in foreign financing in the government budget. The identified fiscal dominance for the sample period, implies a subordinated monetary policy, compromising on Bank of Tanzania’s primary objective of price stability.