bluuebunny/crossref_metadata_2025 huggingface dataset:
Pengaruh Pertumbuhan Penjualan, Intensitas Aset, Kualitas Audit, dan Profitabilitas Terhadap Penghindaran Pajak Perusahaan Pertambangan
Authors: Atikah Filzah Danuarti , Ariani Kurnia Rina
Published: November 2024

Penelitian ini bertujuan untuk mengevaluasi dampak dari pertumbuhan penjualan, intensitas aset, kualitas audit, dan profitabilitas terhadap penghindaran pajak di perusahaan-perusahaan pertambangan yang terdaftar di Bursa Efek Indonesia (BEI) selama periode 2021-2023. Penghindaran pajak diartikan sebagai strategi yang digunakan perusahaan untuk mengurangi kewajiban pajak melalui perencanaan pajak yang sah, meskipun sering kali berdampak pada penurunan penerimaan negara. Metode yang digunakan dalam penelitian ini adalah kuantitatif dengan memanfaatkan data sekunder dari laporan keuangan perusahaan yang terdaftar di BEI. Untuk analisis data, digunakan regresi linier berganda guna mengidentifikasi pengaruh variabel independen yaitu pertumbuhan penjualan, intensitas aset, kualitas audit dan profitabilitas, dan terhadap variabel dependen, yaitu penghindaran pajak. Pengukuran penghindaran pajak dilakukan dengan menggunakan proxy effective tax rate (ETR). Diharapkan hasil penelitian ini dapat memberikan bukti empiris mengenai faktor-faktor yang memengaruhi penghindaran pajak dalam sektor pertambangan di Indonesia, serta menjadi acuan bagi manajemen perusahaan dalam merumuskan strategi pengelolaan pajak.
Harnessing AWS for Transaction Monitoring: A Comprehensive Study on Cloud-Based Anomaly Detection
Authors: Jindal Khushi , Sharma Kusum , Tomar Muskan , Reddy S R N
Published: November 2024

Digital finance has changed how we conduct transactions and opened up new avenues for fraud. This paper proposes an integrated system for the supervision of e-transactions at the bank and detecting possible frauds employing supervised learning techniques by making use of the Amazon SageMaker. Our approach helps solve class imbalance by adjusting weights and employing synthetic data generation methods. One must also tweak the hyperparameters of the models to increase performance levels. Out of all the models examined, Random Forest emerged as the most accurate model that can help improve the security system in banks. The results show also the ability of AI cloud-based solutions such as SageMaker to bolster financial institutions in responding to new cyber threats. What is remarkable is that the system achieves near
Challenges Faced by Cotton Farmers in Adapting to Climate Variability and Proposed Solutions
Authors: Mahesh L. , Ahire R. D. , Deshmukh P. R. , Kadam R. P. , Asewar B. V.
Published: November 2024

This study was carried out in Telangana's Adilabad and Mahabubnagar districts, where 240 farmers were sampled using an ex-post facto research design. Among the challenges faced, price fluctuations were the most significant, with 95.83% of farmers identifying this issue. This was attributed to the absence of a guaranteed minimum support price, which hampers farmers' income and limits their ability to purchase the inputs required for adapting to climate change. To address this, the majority (91.66%) suggested the government implement a minimum support price. Another prevalent issue was the need for drought- resistant crop varieties, noted by 87.50% of farmers.
The Relationship between Technology for the Development of Green Finance and Economic Growth: A Comparison Study between Developed and Middle East Countries
Authors: Adel Eid Hassan Eman , Hosny Diab Shrouk , Fathi Yehya Ahmed Mohamed , Mohamed Kamel Alaa Emad , Shihata Mansour Abanoub Adly , Mohamed Sultan Shreif Samir , El Sharany Abdullah , Ab Del Aleem Darwesh Nesreen Shreif , Del Azeem Mohamed Alaa Hisham Ab , Yassein Ahmed Salma Mohamed , Sattar Mostafa Menna Ab Del
Published: November 2024

This review considers the impact of green economy on the economic growth, the methodology use many different and various indicators, to explain the role of green economy in China, Egypt and Turkey , the paper showed that increasing of the green finance can support the growth positively in the economy in the three countries with different level of implementation.
The impact of ESG strategies on growth in the logistics industry
Authors: Sadowski Adam , Gniadkowska-Szymańska Agata , Sokolovskij Edgar , Jędrzejczak Ryszard
Published: November 2024

The aim of the article is to analyse the relationship between company growth, measured as an increase in Earnings Per Share (EPS) in 3- and 5-year periods, and companies’ financial condition, measured using the Altman z-Score (AS) model. The study was carried out on the example of companies included in the WIG Index and Warsaw Stock Exchange Index (in Polish: Warszawski Indeks Giełdowy – WIG) Environmental, Social, and Governance (ESG) between 2013 and 2020. Furthermore, among the companies included in the WIG index, companies belonging to the logistics industry were distinguished. An analysis of linear and panel relationships was used to verify the nature of the relationships between the variables taken into account. The z-Altman index was found to have a positive effect on company growth in a 3-year period for companies from the transport and logistics industry and all companies included in the WIG ESG index. Regarding company growth over the longer 5-year period, the influence of the z-Altman index on growth was not observed. Therefore, the results for companies in the WIG index show that for company growth in both the 3- and 5-year periods, the financial and economic condition of a company, measured by the z-Altman index, has no impact on the size of this growth, which was also confirmed by panel models.
Correcting Turbulence-induced Errors in Fiber Positioning for the Dark Energy Spectroscopic Instrument
Authors: Schlafly E. F. , Guy J. , Honscheid K. , Kent S. , Koposov S. E. , Aguilar J. , Ahlen S. , Bailey S. , Brooks D. , Claybaugh T. , Dawson K. , Doel P. , Fanning K. , Finkbeiner D. P. , Font-Ribera A. , Forero-Romero J. E. , Gontcho A Gontcho S. , Gutierrez G. , Kirkby D. , Kisner T. , Kremin A. , Landriau M. , Lasker J. , Le Guillou L. , Levi M. E. , de la Macorra A. , Martini P. , Meisner A. , Miquel R. , Moustakas J. , Niz G. , Prada F. , Rossi G. , Sanchez E. , Schubnell M. , Sharples R. , Sprayberry D. , Tarlé G. , Weaver B. A. , Zou H. ,   DESI
Published: November 2024

Highly multiplexed, robotic, fiber-fed spectroscopic surveys are observing tens of millions of stars and galaxies. For many systems, accurate positioning relies on imaging the fibers in the focal plane and feeding that information back to the robotic positioners to correct their positions. Inhomogeneities and turbulence in the air between the focal plane and the imaging camera can affect the measured positions of fibers, limiting the accuracy with which fibers can be placed on targets. For the Dark Energy Spectroscopic Instrument, we dramatically reduced the effect of turbulence on measurements of positioner locations in the focal plane by taking advantage of stationary positioners and the correlation function of the turbulence. We were able to reduce positioning errors from 7.3 to 3.5 μm, speeding the survey by 1.6% under typical conditions.
New Moons of Uranus and Neptune from Ultradeep Pencil-beam Surveys
Authors: Sheppard Scott S. , Tholen David J. , Brozovic Marina , Jacobson Robert , Trujillo Chadwick A. , Lykawka Patryk Sofia , Alexandersen Mike
Published: November 2024

We have conducted extremely ultradeep pencil-beam observations for new satellites around both Uranus and Neptune. Tens of images on several different nights in 2021, 2022, and 2023 were obtained, shifted, and added together to reach as faint as 26.9 and 27.2 mag in the r band around Uranus and Neptune, respectively. One new moon of Uranus, S/2023 U1, and two new moons of Neptune, S/2021 N1 and S/2002 N5, were found. S/2023 U1 was 26.6 mag, is about 7 km in diameter, and has a distant, eccentric, and inclined retrograde orbit similar to Caliban and Stephano, implying these satellites are fragments from a once larger parent satellite. S/2021 N1 was 26.9 mag, about 14 km in size, and has a retrograde orbit similar to Neso and Psamathe, indicating they are a dynamical family. We find S/2021 N1 is in Kozai–Lidov orbital resonance. S/2002 N5 was 25.9 mag, is about 23 km in size, and it makes a family of distant prograde satellites with Sao and Laomedeia. This survey mostly completes the outer satellites of Uranus to about 8 km and Neptune to about 14 km in diameter. The size distributions of satellite dynamical families around the giant planets shows a strong steepening in the power-law size distribution smaller than 5 km in diameter. The satellites of a family become much more common at diameters smaller than 5 km and their size distribution is consistent with a collisional breakup of a once larger parent satellite.
Generating X-Ray Transit Profiles with Batman
Authors: King George W. , Corrales Lía R. , Wheatley Peter J. , Cilley Raven C. , Hollands Mark
Published: November 2024

We present an adaptation of the exoplanet transit model code batman, in order to permit the generation of X-ray transits. Our underlying extended coronal model assumes an isothermal plasma that is radially symmetric. While this ignores the effect of bright, active regions, observations of transits in X-rays will require averaging across multiple epochs of data for the foreseeable future, significantly reducing the importance of more complex modeling. Our publicly available code successfully generates the predicted W-shaped transit profile in X-rays due to the optically thin nature of the emission, which concentrates the expected observational emission around the limb of the photospheric stellar disk. We provide some examples based on the best known X-ray transit target, HD 189733 b, and examine the effect of varying the planet size, coronal temperature, and impact parameter on the resulting transit profile. We also derived scaling relationships for how the overall transit detectability is affected by changing these parameters. Over most of the parameter space, we find that the detectability scales linearly with the cross-sectional area of the planet in X-rays. The relationship with increasing coronal temperature is less fixed, but averages out to a power law with slope −1/4 except when the impact parameter is high. Indeed, varying impact parameter has little effect on detectability at all until it approaches unity.
Acoustic Wake in a Singular Isothermal Profile: Dynamical Friction and Gravitational-wave Emission
Authors: Eytan Gali , Desjacques Vincent , Buehler Robin
Published: November 2024

We consider the motion of a circularly moving perturber in a self-gravitating, collisional system with a spherically symmetric density profile. We concentrate on the singular isothermal sphere, which, despite its pathological features, admits a simple polarization function in linear response theory. This allows us to solve for the acoustic wake trailing the perturber and the resulting dynamical friction, in the limit where the self-gravity of the response can be ignored. In a steady state and for subsonic velocities v

p
< c

s
, the dynamical friction torque

F

φ

∝

v

p

3

is suppressed for perturbers orbiting in an isothermal sphere relative to the infinite, homogeneous medium expectation F

φ
∝ v

p
. For highly supersonic motions, both expectations agree and are consistent with a local approximation to the gravitational torque. At fixed resolution (a given Coulomb logarithm), the response of the system is maximal for Mach numbers near the constant circular velocity of the singular isothermal profile. This resonance maximizes the gravitational-wave (GW) emission produced by the trailing acoustic wake. For an inspiral around a massive black hole of mass 106
M
⊙ located at the center of a (truncated) isothermal sphere, this GW signal could be comparable to the vacuum GW emission of a black hole binary at subnanohertz frequencies when the small black hole enters the Bondi sphere of the massive one. The exact magnitude of this effect depends on departures from hydrostatic equilibrium and on the viscosity present in any realistic astrophysical fluid, which are not included in our simplified description.
Probing the Circumstellar Environment of the Highly Luminous Type IIn Supernova ASASSN-14il
Authors: Dukiya Naveen , Gangopadhyay Anjasha , Misra Kuntal , Hosseinzadeh Griffin , Bostroem K. Azalee , Ailawadhi Bhavya , Howell D. Andrew , Valenti Stefano , Arcavi Iair , McCully Curtis , Gupta Archana
Published: November 2024

We present long-term photometric and spectroscopic studies of circumstellar material (CSM)–ejecta interacting supernova (SN) ASASSN-14il in the galaxy PGC 3093694. The SN reaches a peak r-band magnitude of ∼−20.3 ± 0.2 mag, rivaling SN 2006tf and SN 2010jl. The multiband and the pseudo-bolometric lightcurves show a plateau lasting ∼50 days. Semi-analytical CSM interaction models can match the high luminosity and decline rates of the lightcurves but fail to faithfully represent the plateau region and the bumps in the lightcurves. The spectral evolution resembles a typical Type IIn SN dominated by CSM interaction, showing blue continuum and narrow Balmer lines. The lines are dominated by electron scattering at early epochs. The signatures of the underlying ejecta are visible as the broad component in the Hα profile from as early as day 50, hinting at asymmetry in the CSM. A narrow component is persistent throughout the evolution. The SN shows remarkable photometric and spectroscopic similarity with SN 2015da. However, the different polarization in ASASSN-14il compared to SN 2015da suggests an alternative viewing angle. The late-time blueshift in the Hα profile supports dust formation in the post-shock CSM or ejecta. The mass-loss rate of 2–7 M
⊙ yr−1 suggests a luminous blue variable progenitor in an eruptive phase for ASASSN-14il.
Direct Collapse Accretion Disks within Dark Matter Halos: Saturation of the Magnetorotational Instability and the Field Expulsion
Authors: Luo Yang , Shlosman Isaac
Published: November 2024

We have used high-resolution zoom-in simulations of direct collapse to supermassive black hole (SMBH) seeds within dark mater halos in the presence of magnetic fields generated during the collapse, down to 10−5 pc or 2 au. We confirm an efficient amplification of magnetic field during collapse, the formation of a geometrically thick self-gravitating accretion disk inside 0.1 pc, and damping of fragmentation in the disk by the field. This disk differs profoundly from SMBH accretion disks. We find the following: (1) The accretion disk is subject to the magnetorotational instability, which further amplifies the field to near equipartition. No artificial seeding of the disk field has been used. (2) The equipartition toroidal field changes its polarity in the midplane. (3) The nonlinear Parker instability develops, accompanied by the vertical buckling of the field lines, which injects material above the disk, leading to an increase in the disk scale height. (4) With the Coriolis force producing a coherent helicity above the disk, the vertical poloidal field has been generated and amplified. (5) We estimate that the associated outflow will be most probably squashed by accretion. The resulting configuration consists of a magnetized disk with β ≳ 0.1 and its magnetosphere with β ≪ 1, where β = P
th/P

B
is the ratio of thermal to magnetic energy density. (6) The disk is highly variable, due to feeding by variable accretion flow, and strong vortical motions are present. (7) Finally, the negative gradient of the total vertical stress drives an equatorial outflow sandwiched by an inward accretion flow.
Benchmarking Dielectronic Recombination Rate Coefficients for Carbon-like Ca14+
Authors: Zhang C. Y. , Yan B. S. , Wang K. , Si R. , Yao K. , Ma W. L. , Huang Z. K. , Wen W. Q. , Ma X. W. , Zhu L. F. , Chen C. Y. , Badnell N. R.
Published: November 2024

Dielectronic recombination (DR) rate coefficients for C-like Ca14+ were measured by Wen et al. at the electron cooler storage ring in Lanzhou, China. The measured DR rate coefficients from 0 to 92 eV cover most of the DR resonances associated with the 2s
22p
2 → 2s
22p
2 and 2s
22p
2 → 2s2p
3 core transitions. In addition, Wen et al. reported theoretical results calculated with the Flexible Atomic Code (FAC) and AUTOSTRUCTURE (AS). However, these theoretical results show widespread and significant differences from the measured DR spectrum in both resonance energies and strengths, as well as between each other. In the present work, we uncover the reasons behind these large differences, both theoretical and experimental. The new FAC and AS results reproduce the observed spectrum in detail, especially at resonance energies below 8 eV, and they are in very close agreement with each other. The present plasma rate coefficients agree with the experimentally determined values to within 20% and 2% in the photoionized plasma (PP) and collisional ionized plasma (CP) temperature ranges, respectively. This is in contrast to the previous theoretical results, which showed differences with the experiment of up to ∼40% over the PP temperature range. The present FAC and AS results agree with each other within 5% in the PP and CP temperature ranges. Thus, the theoretical uncertainty is greatly reduced for the DR of Ca14+ and the present benchmarking with the experiment gives confidence to data users modeling non–local thermodynamic equilibrium plasma.
Physical Parameters and Properties of 20 Cold Brown Dwarfs in JWST
Authors: Tu Zhijun , Wang Shu , Liu Jifeng
Published: November 2024

We present a comprehensive analysis of 20 T and Y dwarfs using spectroscopy from the Near-Infrared Spectrograph (NIRSpec) CLEAR/PRISM and Mid-Infrared Instrument (MIRI) low-resolution spectrometer instruments on the James Webb Space Telescope. To characterize the atmospheric parameters, we utilize two atmospheric model grids: the Sonora Elf Owl and ATMO2020++. The effective temperatures derived from the two models are relatively consistent, and metallicities are both close to solar values. However, significant discrepancies are found in other parameters, particularly in surface gravity, with the values obtained from the Sonora Elf Owl models typically being about 1 dex lower than those from the ATMO2020++ models. Further comparisons using the ATMO2020 models highlight that the adiabatic convective process introduced in the ATMO2020++ models has a significant impact on the determination of surface gravity. Using the fitted effective temperatures and absolute parallaxes from the literature, we derive radii for the brown dwarfs, which range from approximately 0.8–1.2 R
Jup. The estimated masses and ages, derived using evolutionary tracks, indicate that most brown dwarfs in our sample have masses below 30 M
Jup and are younger than 6 Gyr. Specifically, Y dwarfs have masses ranging from 2 to 20 M
Jup and ages between 0.1 and 6.7 Gyr. In addition, we discuss the determination of atmospheric parameters using only NIRSpec or MIRI spectra. Comparisons with results from the combined spectra show that the effective temperatures and surface gravities derived solely from NIRSpec spectra are largely consistent with those obtained from the combined spectra.
“Halfway to Rayleigh” and Other Insights into the Rossby Wave Instability
Authors: Chang Eonho , Youdin Andrew N.
Published: November 2024

The Rossby wave instability (RWI) is the fundamental nonaxisymmetric radial shear instability in disks. The RWI can facilitate disk accretion, set the shape of planetary gaps, and produce large vortices. It arises from density and/or temperature features, such as radial gaps, bumps, or steps. A general, sufficient condition to trigger the RWI is lacking, which we address by studying the linear RWI in a suite of simplified models, including incompressible and compressible shearing sheets and global, cylindrical disks. We focus on enthalpy amplitude and width as the fundamental properties of disk features with various shapes. We find analytic results for the RWI boundary and growth rates across a wide parameter space, in some cases with exact derivations and in others as a description of numerical results. Features wider than a scale height generally become unstable about halfway to Rayleigh instability, i.e., when the squared epicyclic frequency is about half the Keplerian value, reinforcing our previous finding. RWI growth rates approximately scale as enthalpy amplitude to the 1/3 power, with a weak dependence on width, across much of the parameter space. Global disk curvature affects wide planetary gaps, making the outer gap edge more susceptible to the RWI. Our simplified models are barotropic and height integrated, but the main results should carry over to more complex and realistic scenarios.
GTC Optical/Near-infrared Upper Limits and NICER X-Ray Analysis of SGR J1935+2154 for the Outburst in 2022
Authors: Shao Yi-Xuan , Zhou Ping , Li Xiang-Dong , Zhang Bin-Bin , Castro-Tirado Alberto Javier , Wang Pei , Li Di , Zhang Zeng-Hua , Zhang Zi-Jian , Hu You-Dong , Pandey Shashi B.
Published: November 2024

The Galactic magnetar SGR J1935+2154 has undergone another outburst since 2022 October 10. We present the results of searching for an optical/near-infrared (NIR) counterpart of SGR J1935+2154 before and during this outburst. No counterpart was detected at the magnetar’s position in

r
′

and

z
′

bands, providing stringent upper limits of

r
′
≳
28.65

and

z
′
≳
26.27

. Using archival X-ray data from NICER, we investigated the properties of the bursts and the spectral evolution of persistent emission. The burst flux F showed a power-law distribution of N ∝ F
−0.76±0.10 for flux ≳2.6 × 10−9erg cm−2 s−1, while the temperature and radius followed a log-normal distribution with

kT
=

1.63

−
0.50

+
0.73

keV

and

R

bb

=

4.35

−
1.35

+
1.95

km

, respectively. The persistent flux evolution experienced a quick decay and an enhancement ∼27 days after the Burst Alert Telescope trigger. Using the NIR and X-ray emission, together with the Gran Telescopio Canarias optical/NIR upper limits, we discussed the origin of the NIR emission from the magnetar based on the fallback disk model and magnetosphere model. We found that either model cannot be ruled out with currently available data. Further mid-infrared observations are needed to find out the mechanism for producing the NIR emission from SGR J1935+2154.
A SPectroscopic Survey of Biased Halos In the Reionization Era (ASPIRE): JWST Supports Earlier Reionization around [O iii] Emitters
Authors: Jin Xiangyu , Yang Jinyi , Fan Xiaohui , Wang Feige , Kakiichi Koki , Meyer Romain A. , Becker George D. , Zou Siwei , Bañados Eduardo , Champagne Jaclyn B. , D’Odorico Valentina , Yue Minghao , Bosman Sarah E. I. , Cai Zheng , Eilers Anna-Christina , Hennawi Joseph F. , Jun Hyunsung D. , Li Mingyu , Li Zihao , Liu 刘 Weizhe 伟哲 , Pudoka Maria , Satyavolu Sindhu , Sun Fengwu , Tee Wei Leong , Wu Yunjing
Published: November 2024

Understanding when and how reionization happened is crucial for studying the early structure formation and the properties of the first galaxies in the Universe. At z > 5.5, the observed intergalactic medium (IGM) optical depth shows a significant scatter, indicating an inhomogeneous reionization process. However, the nature of the inhomogeneous reionization remains debated. A SPectroscopic survey of biased halos In the Reionization Era (ASPIRE) is a JWST Cycle 1 program that has spectroscopically identified >400 [O iii] emitters in 25 quasar fields at z > 6.5. Combined with deep ground-based optical spectroscopy of ASPIRE quasars, the ASPIRE program provides the current largest sample for IGM-galaxy connection studies during cosmic reionization. We present the first results of IGM effective optical depth measurements around [O iii] emitters using 14 ASPIRE quasar fields. We find the IGM transmission is tightly related to reionization era galaxies to the extent that a significant excess of Lyα transmission exists around [O iii] emitters. We measure the stacked IGM effective optical depth of IGM patches associated with [O iii] emitters and find they reach the same IGM effective optical depth at least d
z ∼ 0.1 ahead of those IGM patches where no [O iii] emitters are detected, supporting earlier reionization around [O iii] emitters. Our results indicate an enhancement in IGM Lyα transmission around [O iii] emitters at scales beyond 25 h
−1 cMpc, consistent with the predicted topology of reionization from fluctuating UV background models.
Occurrence of Gravitational Collapse in the Accreting Neutron Stars of Binary-driven Hypernovae
Authors: Becerra L. M. , Cipolletta F. , Fryer C. L. , Menezes Débora P. , Providência Constança , Rueda J. A. , Ruffini R.
Published: November 2024

The binary-driven hypernova (BdHN) model proposes long gamma-ray bursts (GRBs) originate in binaries composed of a carbon–oxygen (CO) star and a neutron star (NS) companion. The CO core collapse generates a newborn NS and a supernova that triggers the GRB by accreting onto the NSs, rapidly transferring mass and angular momentum to them. This article aims to determine the conditions under which a black hole (BH) forms from NS collapse induced by the accretion and the impact on the GRB’s observational properties and taxonomy. We perform three-dimensional, smoothed particle hydrodynamics simulations of BdHNe using up-to-date NS nuclear equations of state, with and without hyperons, and calculate the structure evolution in full general relativity. We assess the binary parameters leading either NS in the binary to the critical mass for gravitational collapse into a BH and its occurrence time, t
col. We include a nonzero angular momentum of the NSs and find that t
col ranges from a few tens of seconds to hours for decreasing NS initial angular momentum values. BdHNe I are the most compact (about 5 minute orbital period), promptly form a BH, and release ≳1052 erg of energy. They form NS–BH binaries with tens of kiloyears merger timescales by gravitational-wave emission. BdHNe II and III do not form BHs, and release ∼1050–1052 erg and ≲1050 erg of energy, respectively. They form NS–NS binaries with a range of merger timescales larger than for NS–BH binaries. In some compact BdHNe II, either NS can become supramassive, i.e., above the critical mass of a nonrotating NS. Magnetic braking by a 1013 G field can delay BH formation, leading to BH–BH or NS–BH with tens of kiloyears merger timescales.
Characterization of Small Flux Ropes Using Juno Spacecraft Cruise-phase Data
Authors: Banu Sahanaj A. , Winslow Réka M. , Scolini Camilla , Davies Emma E. , Farrugia Charles J. , Murphy Amy K. , Lugaz Noé , Al-Haddad Nada
Published: November 2024

In this study, we utilize magnetic field data from the Juno mission’s cruise phase to visually identify and analyze 338 interplanetary small flux ropes (SFRs) across a heliocentric distance range of 1–5.5 au. The events are uniformly distributed across heliocentric distances, showing no clear trend. Through superposed epoch analysis, we find that the average SFR magnetic field profiles are symmetric and show little variation across the observed heliocentric distances. Additionally, we observe a slight increasing trend in the mean duration of SFRs, indicating minimal expansion during propagation. Furthermore, we determine that the SFR mean magnetic field dependence on distance is best fit by two separate power laws, exhibiting a steeper decay from 1 to ∼2.1 au and a shallower decay from ∼2.1 to 5.5 au. Near 1 au, the statistical decay rate of the mean magnetic field magnitude of SFRs is slightly higher than that of the interplanetary magnetic field (IMF), suggesting that SFRs may become indistinguishable from the IMF over time. This finding implies that SFRs detected at greater radial distances are possibly generated in situ as opposed to near the Sun. However, only ∼26% of the total population of SFRs in our catalog occurs within 1 day from the heliospheric current sheet (HCS), indicating a very limited association between the occurrence of the majority of SFRs and the presence of the HCS. These results raise questions about the origin of SFRs detected at larger distances, encouraging further exploration for alternatives to the conventional generation mechanisms.
Constraining the Diffusion Coefficient and Cosmic-Ray Acceleration Efficiency Using Gamma-Ray Emission from the Star-forming Region RCW 38
Authors: Pandey Paarmita , Lopez Laura A. , Rosen Anna L. , Thompson Todd A. , Linden Tim , Blackstone Ian
Published: November 2024

Stellar winds from massive stars may be significant sources of cosmic rays (CRs). To investigate this connection, we report a detailed study of gamma-ray emission near the young Milky Way star cluster (≈0.5 Myr old) in the star-forming region RCW 38 and compare this emission to its stellar wind properties and diffuse X-ray emission. Using 15 yr of Fermi-LAT data in the 0.2–300 GeV band, we find a significant (σ > 22) detection coincident with the star cluster, producing a total gamma-ray luminosity (extrapolated over 0.1–500 GeV) of L

γ
=(2.66 ± 0.92) × 1034 erg s−1 adopting a power-law spectral model (Γ = 2.34 ± 0.04). Using an empirical relationship and STARBURST99, we estimate the total wind power to be 8 × 1036 erg s−1, corresponding to a CR acceleration efficiency of η
CR ≃ 0.4 for an assumed diffusion coefficient consistent with D = 1028 cm2 s−1. Alternatively, a lower acceleration efficiency of 0.1 can produce this L

γ
if the diffusion coefficient is smaller, D ≃ 2.5 × 1027 cm2 s−1. Additionally, we analyze Chandra X-ray data from the region and compare the hot-gas pressure to the CR pressure. We find the former is 4 orders of magnitude greater, suggesting that the CR pressure is not dynamically important relative to stellar winds. As RCW 38 is too young for supernovae to have occurred, the high CR acceleration efficiency in RCW 38 demonstrates that stellar winds may be an important source of Galactic CRs.
Investigating the Kinematics of Central and Satellite Galaxies Using Normalizing Flows
Authors: Kwon K. J. , Hahn ChangHoon
Published: November 2024

Galaxy clustering contains information on cosmology, galaxy evolution, and the relationship between galaxies and their dark matter hosts. On small scales, the detailed kinematics of galaxies within their host halos determines the galaxy clustering. In this paper, we investigate the dependence of the central and satellite galaxy kinematics on
θ
, the intrinsic host halo properties (mass, spin, concentration), cosmology (Ωm, σ
8), and baryonic feedback from active galactic nuclei and supernovae (A
AGN1, A
AGN2, A
SN1, A
SN2). We utilize 2000 hydrodynamic simulations in CAMELS run using IllustrisTNG and SIMBA galaxy formation models. Focusing on central and satellite galaxies with M
* > 109
M
⊙, we apply neural density estimation (NDE) with normalizing flows to estimate their p(Δr ∣
θ
) and p(Δv ∣
θ
), where Δr and Δv are the magnitudes of the halocentric spatial and velocity offsets. With NDE, we accurately capture the dependence of galaxy kinematics on each component of
θ
. For central galaxies, we identify significant spatial and velocity biases dependent on halo mass, concentration, and spin. For satellite distributions, we find significant deviations from a Navarro–Frenk–White profile and evidence that they consist of distinct orbiting and infalling populations. However, we find no strong dependence on
θ
besides a weak dependence on host halo spin. For both central and satellite galaxies, there is no notable dependence on cosmological parameters and baryonic feedback. These results provide key insights for improving the current halo occupation distribution (HOD) models. This work is the first in a series that will reexamine and develop HOD frameworks for improved modeling of galaxy clustering at smaller scales.
Evidence for Abiotic Dimethyl Sulfide in Cometary Matter
Authors: Hänni Nora , Altwegg Kathrin , Combi Michael , Fuselier Stephen A. , De Keyser Johan , Ligterink Niels F. W. , Rubin Martin , Wampfler Susanne F.
Published: November 2024

Technological progress related to astronomical observatories such as the recently launched James Webb Space Telescope (JWST) allows searching for signs of life beyond our solar system, namely, in the form of unambiguous biosignature gases in exoplanetary atmospheres. The tentative assignment of a 1σ–2.4σ spectral feature observed with JWST in the atmosphere of exoplanet K2-18b to the biosignature gas dimethyl sulfide (DMS; sum formula C2H6S) raised hopes that, although controversial, a second genesis had been found. Terrestrial atmospheric DMS is exclusively stemming from marine biological activity, and no natural abiotic source has been identified—neither on Earth nor in space. Therefore, DMS is considered a robust biosignature. Since comets possess a pristine inventory of complex organic molecules of abiotic origin, we have searched high-resolution mass spectra collected at comet 67P/Churyumov–Gerasimenko, target of the European Space Agency’s Rosetta mission, for the signatures of DMS. Previous work reported the presence of a C2H6S signal when the comet was near its equinox, but distinction of DMS from its structural isomer ethanethiol remained elusive. Here we reassess these and evaluate additional data. Based on differences in the electron ionization-induced fragmentation pattern of the two isomers, we show that DMS is significantly better compatible with the observations. Deviations between expected and observed signal intensities for DMS are <1σ, while for ethanethiol they are 2σ–4σ. The local abundance of DMS relative to methanol deduced from these data is (0.13 ± 0.04)%. Our results provide the first evidence for the existence of an abiotic synthetic pathway to DMS in pristine cometary matter and hence motivate more detailed studies of the sulfur chemistry in such matter and its analogs. Future studies need to investigate whether or not the present inference of cometary DMS could provide an abiotic source of DMS in a planetary atmosphere.
Using Polar Faculae to Determine the Sun’s High-latitude Rotation Rate. I. Techniques and Initial Measurements
Authors: Sheeley Neil R.
Published: November 2024

This paper describes a new way of determining the high-latitude solar rotation rate statistically from simultaneous observations of many polar faculae. In this experiment, I extracted frames from a movie made previously from flat-fielded images obtained in the 6767 Å continuum during 1997–1998 February and used those frames to construct spacetime maps from high-latitude slices of the favorably oriented south polar cap. These maps show an array of slanted tracks whose average slope indicates the east–west speed of faculae at that latitude, λ

s
. When the slopes are measured and plotted as a function of latitude, they show relatively little scatter ∼ 0.01–02 km s−1 from a straight line whose zero-speed extension passes through the Sun’s south pole. This means that the speed, v(λ

s
), and the latitudinal radius,

R

⊙

cos

λ

s

, approach 0 at the same rate, so that their ratio gives a nearly constant synodic rotation rate ∼8.°6 day−1 surrounding the Sun’s south pole. A few measurements of the unfavorably oriented north polar cap are consistent with these measurements near the south pole.
Study on the Temporal Evolution of the Radial Differential Rotation of Solar Corona Using Radio Emissions
Authors: Xiang N. B. , Zhao X. H. , Deng L. H. , Li F. Y. , Wang Y. J. , Tan X. W.
Published: November 2024

The daily measurements of the disk-integrated solar radio flux, observed by the Radio Solar Telescope Network, at 245, 410, 610, 1415, 2695, 4995, and 8800 MHz during the time interval of 1989 January 1 to 2019 December 17, are used to investigate the temporal evolution of radial differential rotation of the solar corona using the methods of ensemble empirical mode decomposition (EEMD) and wavelet analysis. Overall, the results reveal that over the 30 yr period, the rotation rates for the observed solar radio flux within the frequency range of 245–8800 MHz show an increase with frequency. This verifies the existence of the radial differential rotation of the solar corona over long timescales of nearly three solar cycles. Based on the radio emission mechanism, to some extent, the results can also serve as an indicator of how the rotation of the solar upper atmosphere varies with altitude within a specific range. From the temporal variation of rotation cycle lengths of radio flux, the coronal rotation at different altitudes from the low corona to approximately 1.3 R
⊙ exhibits complex temporal variations with the progression of the solar cycle. However, in this altitude range, over the past 30 yr from 1989 to 2019, the coronal rotation consistently becomes gradually slower as the altitude increases. Finally, the EEMD method can extract rotation cycle signals from these highly randomized radio emissions, and so it can be used to investigate the rotation periods for the radio emissions at higher or lower frequencies.
Ultra-long-period Cepheids as Standard Candles from Gaia to Rubin-LSST
Authors: Musella Ilaria , Leccia S. , Molinaro R. , Marconi M. , Cusano F. , Di Criscienzo M. , Fiorentino G. , Braga V. , Ripepi V. , De Somma G. , Gatto M. , Luongo E. , Sicignano T.
Published: November 2024

An analysis of the properties of ultra-long-period Cepheids (ULPs) could significantly contribute to understanding the Hubble constant tension, e.g., the current discrepancy between determinations based on local distance indicators and those relying on cosmic microwave background measurements. These highly luminous variables are observable beyond 100 Mpc, so if they were confirmed to behave as standard candles, they would allow us a direct measurement of cosmological distances without any secondary distance indicator, thus reducing potential systematic errors in the calibration of the cosmic distance scale. This paper presents an analysis of the largest known sample of 73 ULPs, including 15 objects in nearby galaxies, with new accurate and homogeneous photometry obtained by Gaia DR3, and a new object, in our Galaxy, identified as a long-period variable in Gaia DR3, but recently reclassified as a ULP. The obtained results suggest that, by improving photometric accuracy, the ULP period–Wesenheit relation shows a smaller dispersion than that obtained in literature and is in better agreement with the classical Cepheid (CC) one, supporting the hypothesis that ULPs are the extension of the CCs at higher period, mass, and luminosity. However, to reach this aim, it is necessary to enrich the sample with high-quality data. The Rubin Observatory Legacy Survey of Space and Time (Rubin-LSST) survey offers the possibility to achieve this thanks to its photometric characteristics and time extension. In particular, we will explore the capabilities of the Rubin-LSST survey to recover ULP theoretical light curves by using a new tool called PulsationStarRecovery, built by our group for this type of analysis.
Invasion and spread of the neotropical leafhopper Curtara insularis (Hemiptera, Cicadellidae) in Africa and North America and the role of high-altitude windborne migration in invasive insects
Authors: Nartey Rita , Chamorro Lourdes , Buffington Matt , Afrane Yaw A. , Mohammed Abdul Rahim , Owusu-Asenso Christopher M. , Akosah-Brempong Gabriel , Pambit-Zong Cosmos M. , Hendrix Solomon V. , Dao Adama , Yaro Alpha S. , Diallo Moussa , Sanogo Zana L. , Djibril Samake , Halbert Susan E. , Bamou Roland , Nance Catherine E. , Bartlett Charles R. , Reynolds Don R. , Chapman Jason W. , Obiri-Danso Kwasi , Lehmann Tovi
Published: November 2024

Invasive insects threaten ecosystem stability, public health, and food security. Documenting newly invasive species and understanding how they reach into new territories, establish populations, and interact with other species remain vitally important. Here, we report on the invasion of the South American leafhopper, Curtara insularis into Africa, where it has established populations in Ghana, encroaching inland at least 350 km off the coast. Importantly, 80% of the specimens collected were intercepted between 160 and 190 m above ground. Further, the fraction of this species among all insects collected was also higher at altitude, demonstrating its propensity to engage in high-altitude windborne dispersal. Its aerial densities at altitude translate into millions of migrants/km over a year, representing massive propagule pressure. Given the predominant south-westerly winds, these sightings suggest an introduction of C. insularis into at least one of the Gulf of Guinea ports. To assess the contribution of windborne dispersal to its spread in a new territory, we examine records of C. insularis range-expansion in the USA. Reported first in 2004 from central Florida, it reached north Florida (Panhandle) by 2008–2011 and subsequently spread across the southeastern and south-central US. Its expansion fits a “diffusion-like” process with 200—300 km long “annual displacement steps”—a pattern consistent with autonomous dispersal rather than vehicular transport. Most “steps” are consistent with common wind trajectories from the nearest documented population, assuming 2—8 hours of wind-assisted flight at altitude. Curtara insularis has been intercepted at US ports and on trucks. Thus, it uses multiple dispersal modalities, yet its rapid overland spread is better explained by its massive propagule pressure linked with its high-altitude windborne dispersal. We propose that high-altitude windborne dispersal is common yet under-appreciated in invasive insect species.
Evaluating spatially explicit management alternatives for an invasive species in a riverine network
Authors: Thompson Brielle K. , Olden Julian D. , Converse Sarah J.
Published: November 2024

Invasive species have substantial ecological and economic costs and removing them can require large investments by management agencies. Optimal spatial allocation of removal effort is critical for efficient and effective management of invasive species. Using a series of ecologically informed model simulations, we evaluated and compared different spatially explicit removal strategies for invasive rusty crayfish (Faxonius rusticus) in the John Day River, USA. We assessed strategies in terms of their performance on three likely management objectives: suppression (minimise overall population abundance), containment (minimise the spatial extent of invasion) and prevention (minimise spread into a specific area). We developed five spatial removal strategies to achieve those objectives, denoted as: Target Abundance (removal at locations with the highest population abundance), Target Growth (removal at locations with the highest population growth), Target Edges (removal at the most distant locations in the river), Target Downstream (removal at the most downstream invaded segments on the Mainstem), and Target Random (removal at randomly selected locations). Each strategy was assessed at various effort levels, referring to the number of spatial segments in the river in which removals were conducted, after seven years of management. We identified the alternative that best achieved each objective, based on decision criteria for risk-neutral and risk-averse decision-makers and further evaluated strategies based on Pareto efficiency, which identifies the set of alternatives for which an improvement on one objective cannot be had without a decline in performance on another. We found that Target Abundance and Target Growth strategies best achieved the suppression objective, for risk neutral and risk averse decision-makers, respectively and Target Downstream was always best in achieving the prevention objective across both types of decision-makers. No single strategy consistently performed best in terms of the containment objective. In terms of all three objectives, Target Downstream was consistently Pareto efficient across all levels of management effort and both decision criteria. The modelling framework we provided is adaptable to a variety of riverine invasive species to help assess and compare spatial management strategies.
Exergía en sistemas energéticos
Authors:   Universidad Autónoma Metropolitana-Iztapalapa, Universidad Autónoma de Nuevo León, México, Espinosa-Paredes Gilberto , Vázquez-Rodríguez Alejandro ,   Universidad Autónoma Metropolitana-Iztapalapa, Universidad Autónoma de Nuevo León, México, Aguilar-Madera Carlos Gilberto ,   Universidad Autónoma Metropolitana-Iztapalapa, Universidad Autónoma de Nuevo León, México
Published: November 2024

Este libro se escribió como material de apoyo para un curso de estudiantes no graduados y proporciona las definiciones y conceptos fundamentales, para la formulación de la Termodinámica enfocada al análisis de Exergía en sistemas diversos, los cuales se encuentran en el entorno del mundo en que vivimos. Este libro trata de la Exergía, como concepto y como una de las propiedades termodinámicas crucial para el análisis de disponibilidad energética en dispositivos ingenieriles y sistemas termodinámicos en general. Además de los principios fundamentales de la Termodinámica, se establece con claridad y sencillez que no es suficiente realizar un análisis termodinámico completo, a menos que se apliquen los conceptos relativos a la exergía. Para comprender los principios básicos de la exergía se presentan soluciones de problemas a través de ejemplos y al final de cada capítulo se ha incluido una selección de preguntas y problemas propuestos para que el estudiante mejore su habilidad en la solución de problemas de cada temática. Con la idea de integrar los conceptos básicos se presenta el análisis exergético de una selección de sistemas energéticos nucleares, geotérmicos, solares y de ciclo combinado.
New concept for the value function of prospect theory
Authors: Sano Kazuo
Published: November 2024

In prospect theory, the value function is typically concave for gains and convex for losses, with losses usually having a steeper slope than gains. The neural system responds differently to losses and gains. Five new studies on neurons related to this issue have examined neuronal responses to losses, gains, and reference points. This study investigated a new concept of the value function. A value function with a neuronal cusp may exhibit variations and behavioral cusps associated with catastrophic events, potentially influencing a trader's decision to close a position. Additionally, we have conducted empirical studies on algorithmic trading strategies that employ different value function specifications.
Conquistas y tesoros de Nueva España y Túnez La recepción de objetos suntuarios foráneos durante el reinado de Carlos V
Authors: Sempere Marín Alicia
Published: November 2024

La llegada a España de objetos de procedencia foránea fue muy intensa durante la primera mitad del siglo XVI. Este artículo ahonda en las posibilidades de estudiar y documentar el origen, motivación, envío, recepción y dispersión de esas remesas aproximándose al análisis de dos célebres conjuntos marcados por circunstancias diversas. En primer lugar, se aborda la problemática recepción y trazabilidad de los obsequios enviados por Hernán Cortés desde Nueva España. A continuación, se documenta el proceso de importación del tesoro de Muley Hassan, rey de Túnez, que se halla entre las posesiones del emperador Carlos V inventariadas tras su muerte, para concluir reflexionando sobre el valor simbólico concedido a los tesoros reales foráneos y su reflejo en la documentación oficial.