bluuebunny/crossref_metadata_2025_split huggingface dataset:
PERENCANAAN STRUKTUR ATAS JEMBATAN CIBUNI DENGAN BETON PRATEGANG PADA KECAMATAN CIJATI KABUPATEN CIANJUR
Authors: Fajriansah Zairofi , Sekaryadi Yudi 
Published: September 2022

AbstrakSTRUCTURAL PLANNING ON CIBUNI BRIDGE WITH PREMATURE CONCRETE IN CIJATI DISTRICT, CIANJUR REGENCYCibuni Bridge is a bridge that connects Cianjur and Sukabumi districts with a span of 30 m and a bridge width of 7 (2x0.5) meters. and the bridge is the only access for the economy of the residents in the area. it is necessary to renew/build a new bridge. The regulations for the design of the loading structure of the Cibuni bridge use the regulations of the Ministry of Public Works RSNI 2016. This plan uses prestressed concrete with predetermined dimensions, including elongated girders using dimensions H-170 cm, with support poles using dimensions of 40 x 12 cm with a distance of each backing pole 200 cm with a height of 100 cm, while the main reinforcement uses 10 mm and stirrup reinforcement -150 mm, the floor plate uses a thickness of 20 cm with the main reinforcement 10 – 200 mm and 13 – 200mm. for the quality of the concrete used on the floor slab of 30 MPa.Keywords: Prestressed Concrete Bridge, Girder Beam, VSL Cable, Superstructure AbstrakJembatan Cibuni adalah jembatan yang menghubungkan antara kabupaten Cianjur dan Kabupaten Sukabumi dengan bentang 30 m dan lebar jembatan 7(2x0,5)meter. dan Jembatan tersebut adalah akses satu-satu bagi perekonomian warga yang ada di daerah tersebut. diperlukan pembaharuan/pembuatan jembatan baru.peraturan untuk perancangan pembebanan struktur atas jembatan cibuni menggunakan peraturan Departemen Pekerjaan Umum RSNI 2016 .perencanaan ini menggunakan beton prategang dengan dimensi-dimensi yang sudah di tentukan,diantaranya gelagar memanjang menggunakan dimensi H-170 cm, dengan tiang sandaran menggunakan dimensi 40 x 12 cm dengan jarak tiap tiang sandaran 200 cm dengan tinggi 100 cm,adapun tulangan utama memakai ∅ 10 mm dan tulangan sengkang ∅-150 mm,plat lantai menggunakan tebal 20 cm dengan tulangan utama ∅ 10 – 200 mm dan ∅ 13 – 200 mm. untuk mutu beton yang di gunakan pada plat lantai 30 mpa.Kata kunci: Jembatan Beton Prategang, Balok Girder, Kabel VSL, Struktur Atas
ACCESS: Confirmation of a Clear Atmosphere for WASP-96b and a Comparison of Light Curve Detrending Techniques
Authors: McGruder Chima D. , López-Morales Mercedes , Kirk James , Espinoza Néstor , Rackham Benjamin V. , Alam Munazza K. , Allen Natalie , Nikolov Nikolay , Weaver Ian C. , Ortiz Ceballos Kevin , Osip David J. , Apai Dániel , Jordán Andrés , Fortney Jonathan J. 
Published: September 2022

Abstract
One of the strongest Na i features was observed in WASP-96b. To confirm this novel detection, we provide a new 475–825 nm transmission spectrum obtained with Magellan/IMACS, which indeed confirms the presence of a broad sodium absorption feature. We find the same result when reanalyzing the 400–825 nm VLT/FORS2 data. We also utilize synthetic data to test the effectiveness of two common detrending techniques: (1) a Gaussian processes (GP) routine, and (2) common-mode correction followed by polynomial correction (CMC+Poly). We find that both methods poorly reproduce the absolute transit depths but maintain their true spectral shape. This emphasizes the importance of fitting for offsets when combining spectra from different sources or epochs. Additionally, we find that, for our data sets, both methods give consistent results, but CMC+Poly is more accurate and precise. We combine the Magellan/IMACS and VLT/FORS2 spectra with literature 800–1644 nm HST/WFC3 spectra, yielding a global spectrum from 400 to 1644 nm. We used the PLATON and Exoretrievals retrieval codes to interpret this spectrum, and find that both yield relatively deeper pressures where the atmosphere is optically thick at log-pressures between

1.3

−
1.1

+
1.0

and

0.29

−
2.02

+
1.86

bars, respectively. Exoretrievals finds solar to supersolar Na i and H2O log-mixing ratios of

−

5.4

−
1.9

+
2.0

and

−

4.5

−
2.0

+
2.0

, respectively, while PLATON finds an overall metallicity of

log

10

(
Z

/

Z

⊙

)
=
−

0.49

−
0.37

+
1.0

dex. Therefore, our findings are in agreement with the literature and support the inference that the terminator of WASP-96b has few aerosols obscuring prominent features in the optical to near-infrared (near-IR) spectrum.
The Rapid Rotation of the Strongly Magnetic Ultramassive White Dwarf EGGR 156
Authors: Williams Kurtis A. , Hermes J. J. , Vanderbosch Zachary P. 
Published: September 2022

Abstract
The distribution of white dwarf rotation periods provides a means for constraining angular momentum evolution during the late stages of stellar evolution, as well as insight into the physics and remnants of double degenerate mergers. Although the rotational distribution of low-mass white dwarfs is relatively well constrained via asteroseismology, that of high-mass white dwarfs, which can arise from either intermediate-mass stellar evolution or white dwarf mergers, is not. Photometric variability in white dwarfs due to rotation of a spotted star is rapidly increasing the sample size of high-mass white dwarfs with measured rotation periods. We present the discovery of 22.4 minute photometric variability in the light curve of EGGR 156, a strongly magnetic, ultramassive white dwarf. We interpret this variability as rapid rotation, and our data suggest that EGGR 156 is the remnant of a double degenerate merger. Finally, we calculate the rate of period change in rapidly-rotating, massive, magnetic WDs due to magnetic dipole radiation. In many cases, including EGGR 156, the period change is not currently detectable over reasonable timescales, indicating that these WDs could be very precise clocks. For the most highly-magnetic, rapidly-rotating massive WDs, such as ZTF J1901+1450 and RE J0317−853, the period change should be detectable and may help constrain the structure and evolution of these exotic white dwarfs.
Revisit of Open Clusters UPK 39, UPK 41, and PHOC 39: A New Binary Open Cluster Found
Authors: Ye Xianhao , Zhao Jingkun , Oswalt Terry D. , Yang Yong , Zhao Gang 
Published: September 2022

Abstract
We investigate the three open clusters near the Aquila Rift cloud, named UPK 39 (c1 hereafter), UPK 41 (c2 hereafter) in Sim et al. (2019), and PHOC 39 (c3 hereafter) in Hunt & Reffert (2021). Using photometric passpands, reddening, and extinction from Gaia DR3, we construct the color-absolute-magnitude diagram. Using isochrone fits, their ages are estimated as 6.3 ± 0.9, 8.1 ± 1.4 and 21.8 ± 2.2 Myr. Their proper motions and radial velocities, estimated using data from Gaia and LAMOST, are very similar. From their orbits, relative distances among them at different times, kinematics, ages, and metallicities, we conclude that c1 and c2 are primordial binary open cluster, which are likely to have been formed at the same time, and c3 may capture c1, c2 in the future.
KODIAQ-Z: Metals and Baryons in the Cool Intergalactic and Circumgalactic Gas at 2.2 ≲ z ≲ 3.6
Authors: Lehner Nicolas , Kopenhafer Claire , O’Meara John M. , Howk J. Christopher , Fumagalli Michele , Prochaska J. Xavier , Acharyya Ayan , O’Shea Brian W. , Peeples Molly S. , Tumlinson Jason , Hummels Cameron B. 
Published: September 2022

Abstract
We present the KODIAQ-Z survey aimed to characterize the cool, photoionized gas at 2.2 ≲ z ≲ 3.6 in 202 H i-selected absorbers with 14.6 ≤

log

N

H

I

< 20 that probe the interface between galaxies and the intergalactic medium (IGM). We find that gas with

14.6
≤
log

N

H

I

<
20

at 2.2 ≲ z ≲ 3.6 can be metal-rich (−1.6 ≲ [X/H] ≲ − 0.2) as seen in damped Lyα absorbers (DLAs); it can also be very metal-poor ([X/H] < − 2.4) or even pristine ([X/H] < − 3.8), which is not observed in DLAs but is common in the IGM. For

16
<
log

N

H

I

<
20

absorbers, the frequency of pristine absorbers is about 1%–10%, while for

14.6
≤
log

N

H

I

≤
16

absorbers it is 10%–20%, similar to the diffuse IGM. Supersolar gas is extremely rare (<1%) at these redshifts. The factor of several thousand spread from the lowest to highest metallicities and large metallicity variations (a factor of a few to >100) between absorbers separated by less than Δv < 500 km s−1 imply that the metals are poorly mixed in

14.6
≤
log

N

H

I

<
20

gas. We show that these photoionized absorbers contribute to about 14% of the cosmic baryons and 45% of the cosmic metals at 2.2 ≲ z ≲ 3.6. We find that the mean metallicity increases with N
H i
, consistent with what is found in z < 1 gas. The metallicity of gas in this column density regime has increased by a factor ∼8 from 2.2 ≲ z ≲ 3.6 to z < 1, but the contribution of the

14.6
≤
log

N

H

I

<
19

absorbers to the total metal budget of the universe at z < 1 is a quarter of that at 2.2 ≲ z ≲ 3.6. We show that FOGGIE cosmological zoom-in simulations have a similar evolution of [X/H] with N
H i
, which is not observed in lower-resolution simulations. In these simulations, very metal-poor absorbers with [X/H] < − 2.4 at z ∼ 2–3 are tracers of inflows, while higher-metallicity absorbers are a mixture of inflows and outflows.
Testing Model-determined Temperatures in the Hyades: A Bayesian Approach
Authors: Jeffery Elizabeth J. , Taylor Benjamin J. , Joner Michael D. 
Published: September 2022

Abstract
Gains in our understanding of stellar evolution over the last century are largely due to improvements in stellar models. One key aspect in the use of these models is a reliable transformation between theoretical values (such as luminosity and temperature) to observable quantities (such as magnitude and color). To assess the current state of this transformation, we sought to compare model-determined temperatures from color–magnitude diagram fitting to temperatures obtained from photometric colors or spectroscopy. Our sample for analysis was 88 nonbinary stars in the Hyades open star cluster. By applying a sophisticated Bayesian algorithm we fit five widely available model sets to high-quality photometric data combined with Gaia parallaxes. This analysis provides specific feedback for improving temperature–color transformations, as well as practical guidance for using results based on these models.
Characterization of the Fireballs Detected by All-sky Cameras in Romania
Authors: Boaca Ioana , Gritsevich Maria , Birlan Mirel , Nedelcu Alin , Boaca Tudor , Colas François , Malgoyre Adrien , Zanda Brigitte , Vernazza Pierre 
Published: September 2022

Abstract
Some of the fields of research that have captured the persistent interest of both scientists and the general public are meteor phenomena. The main goal in the study of meteoroid impacts into Earth’s atmosphere is the recovery of the remnant matter after the ablation in the form of meteorites. This is a complementary approach, yet cheap alternative, to a sample return mission. Meteoroids are messengers since the time of the formation of the solar system due to the fact that they have preserved the same composition. The study of meteorites provides information regarding the chemical composition from which the planets formed. The increasing number of all-sky camera networks in recent years has resulted in a large set of events available for study. Thus, it is very important to use a method that determines whether the meteoroid could produce a meteorite or not. In this paper we study the meteors detected by the FRIPON network in Romania with the use of all-sky cameras. We focus on the events with noticeable deceleration (V

f
/V
0 < 0.8). We determine the ballistic coefficient α and the mass-loss parameter β for the selected sample. Based on this analysis the events are classified in three categories: (1) meteoroids that are likely to produce meteorites; (2) meteoroids that can possibly produce meteorites; (3) meteoroids that are unlikely to produce meteorites. The entry and final mass are determined for each event. From the recorded fireballs, we identified one possible meteorite dropper, and we analyzed its dynamical evolution.
Deep Two-phase, Hemispherical Magma Oceans on Lava Planets
Authors: Boukaré Charles-Édouard , Cowan Nicolas B. , Badro James 
Published: September 2022

Abstract
Astronomers have discovered a handful of exoplanets with rocky bulk compositions but orbiting that orbit so close to their host star that the surface of the planet must be at least partially molten. It is expected that the dayside of such “lava planets” harbors a rock-vapor atmosphere that flows quickly toward the airless nightside—this partial atmosphere is critical to the interpretation of lava planet observations, but transports negligible heat toward the nightside. As a result, the surface temperature of the magma ocean may range from 3000 K near the substellar point down to 1500 K near the day–night terminator. We use simple models incorporating the thermodynamics and geochemistry of partial melt to predict the physical and chemical properties of the magma ocean as a function of the distance from the substellar point. Our principal findings are that: (1) the dayside magma ocean is much deeper than previously thought, probably extending down to the core–mantle boundary below the substellar point of an Earth-sized planet; (2) much of the dayside is only partially molten, leading to gradients in the surface chemistry of the magma ocean; and (3) the temperature at the base of the silicate mantle is as important as the surface temperature. In the most extreme cases, lava planet interiors could be cold enough such that thermal stratification below the substellar point is gravitationally stable. These findings have important implications for the dynamics of the magma ocean, as well as the composition and dynamics of the atmosphere.
A Nonlocal Magneto-curvature Instability in a Differentially Rotating Disk
Authors: Ebrahimi Fatima , Pharr Matthew 
Published: September 2022

Abstract
A global mode is shown to be unstable to nonaxisymmetric perturbations in a differentially rotating Keplerian disk containing either vertical or azimuthal magnetic fields. In an unstratified cylindrical disk model, using both global eigenvalue stability analysis and linear global initial-value simulations, it is demonstrated that this instability dominates at strong magnetic fields where local standard magnetorotational instability (MRI) becomes stable. Unlike the standard MRI mode, which is concentrated in the high flow shear region, these distinct global modes (with low azimuthal mode numbers) are extended in the global domain and are Alfvén-continuum-driven unstable modes. As its mode structure and relative dominance over MRI are inherently determined by the global spatial curvature as well as the flow shear in the presence of a magnetic field, we call it the magneto-curvature (magneto-spatial-curvature) instability. Consistent with the linear analysis, as the field strength is increased in the nonlinear simulations, a transition from MRI-driven turbulence to a state dominated by global nonaxisymmetric modes is obtained. This global instability could therefore be a source of nonlinear transport in accretion disks at a higher magnetic field than predicted by local models.
Exoplanet Radio Transits as a Probe for Exoplanetary Magnetic Fields—Time-dependent MHD Simulations
Authors: Hazra Soumitra , Cohen Ofer , Sokolov Igor V. 
Published: September 2022

Abstract
We perform a series of time-dependent magnetohydrodynamic simulations of the HD 189733 star–planet system in order to predict radio transit modulations due to the interaction between the stellar wind and planetary magnetic field. The simulation combines a model for the stellar corona and wind with an exoplanet that is orbiting the star in a fully dynamic, time-dependent manner. Our simulations generate synthetic radio images that enable us to obtain synthetic radio light curves in different frequencies. We find a clear evidence for the planetary motion in the radio light curves. Moreover, we find specific repeated features in the light curves that are attributed to the passage of the planetary magnetosphere in front of the star during transit. More importantly, we find a clear dependence in magnitude and phase of these light-curve features on the strength of the planetary magnetic field. Our work demonstrates that if radio transits could be observed, they could indeed provide information about the magnetic field strength of the transiting exoplanet. Future work to parameterize these light-curve features and their dependence on the planetary field strength would provide tools to search for these features in radio observation data sets. As we only consider the thermal radio emission from the host star for our study, very sensitive radio interferometers are necessary to detect these kinds of planetary transits in radio.
The Ultraviolet C ii Lines as a Diagnostic of κ-distributed Electrons in Planetary Nebulae
Authors: Yao Zheng-Wei , Zhang Yong 
Published: September 2022

Abstract
Non-Maxwellian κ electron energy distributions (EEDs) have been proposed in recent years to resolve the so-called “electron temperature and abundance discrepancy problem” in the study of planetary nebulae (PNs). Thus the need to develop diagnostic tools to determine from observations the EED of PNs is raised. Arising from high-energy levels, the ultraviolet (UV) emission lines from PNs present intensities that depend sensitively on the high-energy tail of the EED. In this work, we investigate the feasibility of using the C ii]λ2326/C ii
λ1335 intensity ratios as a diagnostic of the deviation of the EED from the Maxwellian distribution (as represented by the κ index). We use a Maxwellian decomposition approach to derive the theoretical κ-EED-based collisionally excited coefficients of C ii, and then compute the C ii UV intensity ratio as a function of the κ index. We analyze the archival spectra acquired by the International Ultraviolet Explorer and measure the intensities of C ii UV lines from 12 PNs. By comparing the observed line ratios and the theoretical predictions, we can infer their κ values. With the Maxwellian-EED hypothesis, the observed C ii]λ2326/C ii
λ1335 ratios are found to be generally lower than those predicted from the observed optical spectra. This discrepancy can be explained in terms of the κ EED. Our results show that the κ values inferred range from 15 to infinity, suggesting a mild or modest deviation from the Maxwellian distribution. However, the κ-distributed electrons are unlikely to exist throughout the whole nebulae. A toy model shows that if just about 1%–5% of the free electrons in a PN had a κ EED as small as κ = 3, it would be sufficient to account for the observations.
A Supercritical Accretion Disk with Radiation-driven Outflows
Authors: Cao Xinwu , Gu Wei-Min 
Published: September 2022

Abstract
Outflows are inevitably driven from the disk if the vertical component of the black hole (BH) gravity cannot resist the radiation force. We derive the mass-loss rate in the outflows by solving a dynamical equation for the vertical gas motion in the disk. The structure of a supercritical accretion disk is calculated with the radial energy advection included. We find that most inflowing gas is driven into outflows if the disk is accreting at a moderate Eddington-scaled rate (up to ∼100) at its outer edge, i.e., only a small fraction of gas is accreted by the BH, which is radiating at several Eddington luminosities, while it reaches around ten for extremely high accretion rate cases (

m

̇

≡

M

̇

/

M

̇

Edd

∼
1000

). Compared with a normal slim disk, the disk luminosity is substantially suppressed due to the mass loss in the outflows. We apply the model to the light curves of the tidal disruption events (TDEs) and find that the disk luminosity declines very slowly with time even if a typical accretion rate

m

̇

∝

t

−
5

/

3

is assumed at the outer edge of the disk, which is qualitatively consistent with the observed light curves in some TDEs and helps us to understand the energy deficient phenomenon observed in the TDEs. Strong outflows from supercritical accretion disks surrounding supermassive BHs may play crucial roles in their host galaxies, which can be taken as an ingredient in the mechanical feedback models. The implications of the results on the growth of supermassive BHs are also discussed.
The GALPROP Cosmic-ray Propagation and Nonthermal Emissions Framework: Release v57
Authors: Porter T. A. , Jóhannesson G. , Moskalenko I. V. 
Published: September 2022

Abstract
The past decade has brought impressive advances in the astrophysics of cosmic rays (CRs) and multiwavelength astronomy, thanks to the new instrumentation launched into space and built on the ground. Modern technologies employed by those instruments provide measurements with unmatched precision, enabling searches for subtle signatures of dark matter and new physics. Understanding the astrophysical backgrounds to better precision than the observed data is vital in moving to this new territory. A state-of-the-art CR propagation code, called GalProp, is designed to address exactly this challenge. Having 25 yr of development behind it, the GalProp framework has become a de facto standard in the astrophysics of CRs, diffuse photon emissions (radio to γ-rays), and searches for new physics. GalProp uses information from astronomy, particle physics, and nuclear physics to predict CRs and their associated emissions self-consistently, providing a unifying modeling framework. The range of its physical validity covers 18 orders of magnitude in energy, from sub-keV to PeV energies for particles and from μeV to PeV energies for photons. The framework and the data sets are public and are extensively used by many experimental collaborations and by thousands of individual researchers worldwide for interpretation of their data and for making predictions. This paper details the latest release of the GalProp framework and updated cross sections, further developments of its initially auxiliary data sets for models of the interstellar medium that grew into independent studies of the Galactic structure—distributions of gas, dust, radiation, and magnetic fields—as well as the extension of its modeling capabilities. Example applications included with the distribution illustrating usage of the new features are also described.
Integrated Geostationary Solar Energetic Particle Events Catalog: GSEP
Authors: Rotti Sumanth , Aydin Berkay , Georgoulis Manolis K. , Martens Petrus C. 
Published: September 2022

Abstract
We present a catalog of solar energetic particle (SEP) events covering solar cycles 22, 23 and 24. We correlate and integrate three existing catalogs based on Geostationary Operational Environmental Satellite integral proton flux data. We visually verified and labeled each event in the catalog to provide a homogenized data set. We have identified a total of 341 SEP events of which 245 cross the Space Weather Prediction Center threshold of a significant proton event. The metadata consists of physical parameters and observables concerning the possible source solar eruptions, namely flares and coronal mass ejections for each event. The sliced time-series data of each event, along with intensity profiles of proton fluxes in several energy bands, have been made publicly available. This data set enables researchers in machine learning and statistical analysis to understand the SEPs and the source eruption characteristics useful for space weather prediction.