bluuebunny/crossref_metadata_2025_split huggingface dataset:
Making the Solar System
Authors: Chambers John 
Published: February 2023

Abstract
We model the early stages of planet formation in the solar system, including continual planetesimal formation, and planetesimal and pebble accretion onto planetary embryos in an evolving disk driven by a disk wind. The aim is to constrain aspects of planet formation that have large uncertainties by matching key characteristics of the solar system. The model produces a good fit to these characteristics for a narrow range of parameter space. Planetary growth beyond the ice line is dominated by pebble accretion. Planetesimal accretion is more important inside the ice line. Pebble accretion inside the ice line is slowed by higher temperatures, partial removal of inflowing pebbles by planetesimal formation and pebble accretion further out in the disk, and increased radial velocities due to gas advection. The terrestrial planets are prevented from accreting much water ice because embryos beyond the ice line reach the pebble-isolation mass before the ice line enters the terrestrial-planet region. When only pebble accretion is considered, embryos typically remain near their initial mass or grow to the pebble-isolation mass. Adding planetesimal accretion allows Mars-sized objects to form inside the ice line, and allows giant-planet cores to form over a wider region beyond the ice line. In the region occupied by Mercury, pebble Stokes numbers are small. This delays the formation of embryos and stunts their growth, so that only low-mass planets can form here.
RC100: Rotation Curves of 100 Massive Star-forming Galaxies at z = 0.6–2.5 Reveal Little Dark Matter on Galactic Scales
Authors: Nestor Shachar A. , Price S. H. , Förster Schreiber N. M. , Genzel R. , Shimizu T. T. , Tacconi L. J. , Übler H. , Burkert A. , Davies R. I. , Dekel A. , Herrera-Camus R. , Lee L. L. , Liu D. , Lutz D. , Naab T. , Neri R. , Renzini A. , Saglia R. , Schuster K. F. , Sternberg A. , Wisnioski E. , Wuyts S. 
Published: February 2023

Abstract
We analyze Hα or CO rotation curves extending out to several galaxy effective radii for 100 massive, large, star-forming disk galaxies (SFGs) across the peak of cosmic galaxy star formation (z ∼ 0.6–2.5), more than doubling the previous sample presented by Genzel et al. and Price et al. The observations were taken with SINFONI and KMOS integral-field spectrographs at the ESO-Very Large Telescope, LUCI-LBT, NOEMA-IRAM, and Atacama Large Millimeter/submillimeter Array. We fit the major-axis kinematics with beam-convolved, forward models of turbulent rotating disks with bulges embedded in dark matter (DM) halos, including the effects of pressure support. The fraction of dark to total matter within the disk effective radius (R
e ∼ 5 kpc), f
DM(R
e) = V
2
DM(R
e)/V
2
circ(R
e) decreases with redshift: at z ∼ 1 (z ∼ 2) the median DM fraction is 0.38 ± 0.23 (0.27 ± 0.18), and a third (half) of all galaxies are maximal disks with f
DM(R
e) < 0.28. DM fractions correlate inversely with the baryonic surface density, and the low DM fractions can be explained with a flattened, or cored, inner DM density distribution. At z ∼ 2, there is ≈40% less DM mass on average within R
e compared to expected values based on cosmological stellar-mass–halo-mass relations. The DM deficit is more evident at high star formation rate surface densities (≳2.5 M
⊙ yr−1 kpc2) and galaxies with massive bulges (≥1010
M
⊙). A combination of stellar or active galactic nucleus feedback, and/or heating due to dynamical friction, may drive the DM from cuspy into cored mass distributions, pointing to an efficient buildup of massive bulges and central black holes at z ∼ 2 SFGs.
On the Generation and Evolution of Switchbacks and the Morphology of the Alfvénic Transition: Low Mach-number Boundary Layers
Authors: Liu Ying D. , Ran Hao , Hu Huidong , Bale Stuart D. 
Published: February 2023

Abstract
We investigate the generation and evolution of switchbacks (SBs), the nature of the sub-Alfvénic wind observed by the Parker Solar Probe (PSP), and the morphology of the Alfvénic transition, all of which are key issues in solar wind research. First we highlight a special structure in the pristine solar wind, termed a low Mach-number boundary layer (LMBL). An increased Alfvén radius and suppressed SBs are observed within an LMBL. A probable source on the Sun for an LMBL is the peripheral region inside a coronal hole with rapidly diverging open fields. The sub-Alfvénic wind detected by PSP is an LMBL flow by nature. The similar origin and similar properties of the sub-Alfvénic intervals favor a wrinkled surface for the morphology of the Alfvénic transition. We find that a larger deflection angle tends to be associated with a higher Alfvén Mach number. The magnetic deflections have an origin well below the Alfvén critical point, and deflection angles larger than 90° seem to occur only when M
A ≳ 2. The velocity enhancement in units of the local Alfvén speed generally increases with the deflection angle, which is explained by a simple model. A nonlinearly evolved, saturated state is revealed for SBs, where the local Alfvén speed is roughly an upper bound for the velocity enhancement. In the context of these results, the most promising theory on the origin of SBs is the model of expanding waves and turbulence, and the patchy distribution of SBs is attributed to modulation by reductions in the Alfvén Mach number. Finally, a picture of the generation and evolution of SBs is created based on the results.
The Modulation of Anomalous and Galactic Cosmic-Ray Oxygen over Successive Solar Cycle Minima
Authors: Strauss R. D. , Leske R. A. , Rankin J. S. 
Published: February 2023

Abstract
Both the recent 2009 and 2020 solar minima were classified as unusually quiet and characterized with unusually high galactic cosmic-ray (GCR) levels. However, unlike the trends from previous decades, in which anomalous cosmic-ray (ACR) and GCR levels strongly agreed, the ACR intensities did not reach such high, record-setting levels. This discrepancy between the behavior of GCRs and ACRs is investigated in this work by simulating the acceleration and transport of GCR and ACR oxygen under different transport conditions. After using recent observations to constrain any remaining free parameters present in the model, we show that less turbulent conditions are characterized by higher GCR fluxes and lower ACR fluxes, due to less efficient ACR acceleration at the solar wind termination shock. We offer this as an explanation for the ACR/GCR discrepancy observed during 2009 and 2020, when compared to previous solar cycles.
High-redshift JWST Observations and Primordial Non-Gaussianity
Authors: Biagetti Matteo , Franciolini Gabriele , Riotto Antonio 
Published: February 2023

Abstract
Several bright and massive galaxy candidates at high redshifts have been recently observed by the James Webb Space Telescope. Such early massive galaxies seem difficult to reconcile with standard Λ cold dark matter model predictions. We discuss under which circumstances such observed massive galaxy candidates can be explained by introducing primordial non-Gaussianity in the initial conditions of cosmological perturbations.
A Comprehensive Study of Galaxies at z ∼ 9–16 Found in the Early JWST Data: Ultraviolet Luminosity Functions and Cosmic Star Formation History at the Pre-reionization Epoch
Authors: Harikane Yuichi , Ouchi Masami , Oguri Masamune , Ono Yoshiaki , Nakajima Kimihiko , Isobe Yuki , Umeda Hiroya , Mawatari Ken , Zhang Yechi 
Published: February 2023

Abstract
We conduct a comprehensive study on dropout galaxy candidates at z ∼ 9–16 using the first 90 arcmin2 James Webb Space Telescope (JWST) Near Infrared Camera images taken by the early release observations (ERO) and early release science programs. With the JWST simulation images, we find that a number of foreground interlopers are selected with a weak photo-z determination (Δχ
2 > 4). We thus carefully apply a secure photo-z selection criterion (Δχ
2 > 9) and conventional color criteria with confirmations of the ERO Near Infrared Spectrograph spectroscopic redshifts, and obtain a total of 23 dropout galaxies at z ∼ 9–16, including two candidates at

z

phot

=

16.25

−
0.46

+
0.24

and

16.41

−
0.55

+
0.66

. We perform thorough comparisons of dropout galaxies found in our work with recent JWST studies, and conclude that our galaxy sample is reliable enough for statistical analyses. We derive the UV luminosity functions at z ∼ 9–16, and confirm that our UV luminosity functions at z ∼ 9 and 12 agree with those determined by other Hubble Space Telescope and JWST studies. The cosmic star formation rate (SFR) density decreases from z ∼ 9 to 12, and perhaps to 16, but the densities at z ∼ 12–16 are higher than the constant star formation efficiency model. Interestingly, there are six bright galaxy candidates at z ∼ 10–16 with M
UV < −19.5 mag and M
* ∼ 108−9
M
⊙. Because a majority (∼80%) of these galaxies show no signatures of active galactic nuclei in their morphologies, the high cosmic SFR densities and the existence of these UV-luminous galaxies are explained by the lack of suppression of star formation by the UV background radiation at the pre-reionization epoch and/or an efficient UV radiation production by a top-heavy initial mass function with Population III–like star formation.
Updated Void Catalogs of the SDSS DR7 Main Sample
Authors: Douglass Kelly A. , Veyrat Dahlia , BenZvi Segev 
Published: February 2023

Abstract
We produce several public void catalogs using a volume-limited subsample of the Sloan Digital Sky Survey Data Release 7 (SDSS DR7). Using new implementations of three different void-finding algorithms, VoidFinder and two ZOBOV-based algorithms (VIDE and REVOLVER), we identify 1163, 531, and 518 cosmic voids with radii >10 h
−1 Mpc, respectively, out to a redshift of z = 0.114 assuming a Planck 2018 cosmology, and 1184, 535, and 519 cosmic voids assuming a WMAP5 cosmology. We compute effective radii and centers for all voids and find none with an effective radius >54 h
−1 Mpc. The median void effective radius is 15–19 h
−1 Mpc for all three algorithms. We extract and discuss several properties of the void populations, including radial density profiles, the volume fraction of the catalog contained within voids, and the fraction of galaxies contained within voids. Using 64 mock galaxy catalogs created from the Horizon Run 4 N-body simulation, we compare simulated and observed void properties and find good agreement between the SDSS DR7 and mock catalog results.
PHANGS–JWST First Results: The 21 μm Compact Source Population
Authors: Hassani Hamid , Rosolowsky Erik , Leroy Adam K. , Boquien Médéric , Lee Janice C. , Barnes Ashley T. , Belfiore Francesco , Bigiel F. , Cao Yixian , Chevance Mélanie , Dale Daniel A. , Egorov Oleg V. , Emsellem Eric , Faesi Christopher M. , Grasha Kathryn , Kim Jaeyeon , Klessen Ralf S. , Kreckel Kathryn , Kruijssen J. M. Diederik , Larson Kirsten L. , Meidt Sharon E. , Sandstrom Karin M. , Schinnerer Eva , Thilker David A. , Watkins Elizabeth J. , Whitmore Bradley C. , Williams Thomas G. 
Published: February 2023

Abstract
We use PHANGS–James Webb Space Telescope (JWST) data to identify and classify 1271 compact 21 μm sources in four nearby galaxies using MIRI F2100W data. We identify sources using a dendrogram-based algorithm, and we measure the background-subtracted flux densities for JWST bands from 2 to 21 μm. Using the spectral energy distribution (SED) in JWST and HST bands plus ALMA and MUSE/VLT observations, we classify the sources by eye. Then we use this classification to define regions in color–color space and so establish a quantitative framework for classifying sources. We identify 1085 sources as belonging to the ISM of the target galaxies with the remainder being dusty stars or background galaxies. These 21 μm sources are strongly spatially associated with H ii regions (>92% of sources), while 74% of the sources are coincident with a stellar association defined in the HST data. Using SED fitting, we find that the stellar masses of the 21 μm sources span a range of 102–104
M
⊙ with mass-weighted ages down to 2 Myr. There is a tight correlation between attenuation-corrected Hα and 21 μm luminosity for L

ν,F2100W > 1019 W Hz−1. Young embedded source candidates selected at 21 μm are found below this threshold and have M
⋆ < 103
M
⊙.
PHANGS–JWST First Results: Measuring Polycyclic Aromatic Hydrocarbon Properties across the Multiphase Interstellar Medium
Authors: Chastenet Jérémy , Sutter Jessica , Sandstrom Karin , Belfiore Francesco , Egorov Oleg V. , Larson Kirsten L. , Leroy Adam K. , Liu Daizhong , Rosolowsky Erik , Thilker David A. , Watkins Elizabeth J. , Williams Thomas G. , Barnes Ashley. T. , Bigiel F. , Boquien Médéric , Chevance Mélanie , Dale Daniel A. , Kruijssen J. M. Diederik , Emsellem Eric , Grasha Kathryn , Groves Brent , Hassani Hamid , Hughes Annie , Kreckel Kathryn , Meidt Sharon E. , Pan Hsi-An , Querejeta Miguel , Schinnerer Eva , Whitcomb Cory M. 
Published: February 2023

Abstract
Ratios of polycyclic aromatic hydrocarbon (PAH) vibrational bands are a promising tool for measuring the properties of the PAH population and their effect on star formation. The photometric bands of the MIRI and NIRCam instruments on JWST provide the opportunity to measure PAH emission features across entire galaxy disks at unprecedented resolution and sensitivity. Here we present the first results of this analysis in a sample of three nearby galaxies: NGC 628, NGC 1365, and NGC 7496. Based on the variations observed in the 3.3, 7.7, and 11.3 μm features, we infer changes to the average PAH size and ionization state across the different galaxy environments. High values of F335MPAH/F1130W and low values of F1130W/F770W are measured in H ii regions in all three galaxies. This suggests that these regions are populated by hotter PAHs, and/or that the PAH ionization fraction is larger. We see additional evidence of heating and/or changes in PAH size in regions with higher molecular gas content as well as increased ionization in regions with higher Hα intensity.
PHANGS–JWST First Results: Mapping the 3.3 μm Polycyclic Aromatic Hydrocarbon Vibrational Band in Nearby Galaxies with NIRCam Medium Bands
Authors: Sandstrom Karin M. , Chastenet Jérémy , Sutter Jessica , Leroy Adam K. , Egorov Oleg V. , Williams Thomas G. , Bolatto Alberto D. , Boquien Médéric , Cao Yixian , Dale Daniel A. , Lee Janice C. , Rosolowsky Erik , Schinnerer Eva , Barnes Ashley. T. , Belfiore Francesco , Bigiel F. , Chevance Mélanie , Grasha Kathryn , Groves Brent , Hassani Hamid , Hughes Annie , Klessen Ralf S. , Kruijssen J. M. Diederik , Larson Kirsten L. , Liu Daizhong , Lopez Laura A. , Meidt Sharon E. , Murphy Eric J. , Sormani Mattia C. , Thilker David A. , Watkins Elizabeth J. 
Published: February 2023

Abstract
We present maps of the 3.3 μm polycyclic aromatic hydrocarbon (PAH) emission feature in NGC 628, NGC 1365, and NGC 7496 as observed with the Near-Infrared Camera imager on JWST from the PHANGS–JWST Cycle 1 Treasury project. We create maps that isolate the 3.3 μm PAH feature in the F335M filter (F335MPAH) using combinations of the F300M and F360M filters for removal of starlight continuum. This continuum removal is complicated by contamination of the F360M by PAH emission and variations in the stellar spectral energy distribution slopes between 3.0 and 3.6 μm. We modify the empirical prescription from Lai et al. to remove the starlight continuum in our highly resolved galaxies, which have a range of starlight- and PAH-dominated lines of sight. Analyzing radially binned profiles of the F335MPAH emission, we find that between 5% and 65% of the F335M intensity comes from the 3.3 μm feature within the inner 0.5 r
25 of our targets. This percentage systematically varies from galaxy to galaxy and shows radial trends within the galaxies related to each galaxy’s distribution of stellar mass, interstellar medium, and star formation. The 3.3 μm emission is well correlated with the 11.3 μm PAH feature traced with the MIRI F1130W filter, as is expected, since both features arise from C–H vibrational modes. The average F335MPAH/F1130W ratio agrees with the predictions of recent models by Draine et al. for PAHs with size and charge distributions shifted toward larger grains with normal or higher ionization.
Multi-messenger Model for the Prompt Emission from GRB 221009A
Authors: Rudolph Annika , Petropoulou Maria , Winter Walter , Bošnjak Željka 
Published: February 2023

Abstract
We present a multi-messenger model for the prompt emission from GRB 221009A within the internal shock scenario. We consider the time-dependent evolution of the outflow with its impact on the observed light curve from multiple collisions, as well as the self-consistent generation of the electromagnetic spectrum in synchrotron and inverse Compton-dominated scenarios. Our lepto-hadronic model includes UHE protons potentially accelerated in the outflow, and their feedback on spectral energy distribution and on the neutrino emission. We find that we can roughly reproduce the observed light curves with an engine with varying ejection velocity of ultrarelativistic material, which has an intermediate quiescent period of about 200 s and a variability timescale of ∼1 s. We consider baryonic loadings of 3 and 30 that are compatible with the hypothesis that the highest-energetic LHAASO photons might come from UHECR interactions with the extragalactic background light, and the paradigm that energetic GRBs may power the UHECR flux. For these values and the high dissipation radii considered, we find consistency with the nonobservation of neutrinos and no significant signatures on the electromagnetic spectrum. Inverse Compton-dominated scenarios from the prompt emission are demonstrated to lead to about an order of magnitude higher fluxes in the HE range; this enhancement is testable via its spectral impact in the Fermi-GBM and LAT ranges.
Exploring the Chemical Evolution of Nitrogen and Oxygen in Local Star-forming Galaxies
Authors: Stephenson Mabel G. , Arellano-Córdova Karla Z. , Berg Danielle A. , Mingozzi Matilde , James Bethan L. 
Published: February 2023

Abstract
We utilize a sample of 45 local star-forming galaxies (z < 0.18) from the COS Legacy Archive Spectroscopic SurveY (CLASSY) to analyze the N/O versus O/H relationship. Nitrogen and oxygen are ejected into the interstellar medium at different timescales by intermediate-mass and massive stars. Therefore, the N/O abundance ratio with respect to the gas-phase metallicity (O/H) is a powerful tool to improve our interpretation on galaxy formation and evolution. In order to analyze such a relation, we derive the the electron density and temperature for the whole sample, allowing for accurate determinations of N/O and the metallicity. We compare our results with an additional sample of dwarf star-forming galaxies and extragalactic H ii regions. We also analyze the N/O ratio with the stellar mass and star formation rate.
Io’s Optical Aurorae in Jupiter’s Shadow
Authors: Schmidt Carl , Sharov Mikhail , de Kleer Katherine , Schneider Nick , de Pater Imke , Phipps Phillip H. , Conrad Albert , Moore Luke , Withers Paul , Spencer John , Morgenthaler Jeff , Ilyin Ilya , Strassmeier Klaus , Veillet Christian , Hill John , Brown Mike 
Published: February 2023

Abstract
Decline and recovery timescales surrounding eclipse are indicative of the controlling physical processes in Io’s atmosphere. Recent studies have established that the majority of Io’s molecular atmosphere, SO2 and SO, condenses during its passage through Jupiter’s shadow. The eclipse response of Io’s atomic atmosphere is less certain, having been characterized solely by ultraviolet aurorae. Here we explore the response of optical aurorae for the first time. We find oxygen to be indifferent to the changing illumination, with [O i] brightness merely tracking the plasma density at Io’s position in the torus. In shadow, line ratios confirm sparse SO2 coverage relative to O, since their collisions would otherwise quench the emission. Io’s sodium aurora mostly disappears in eclipse and e-folding timescales, for decline and recovery differ sharply: ∼10 minutes at ingress and nearly 2 hr at egress. Only ion chemistry can produce such a disparity; Io’s molecular ionosphere is weaker at egress due to rapid recombination. Interruption of a NaCl+ photochemical pathway best explains Na behavior surrounding eclipse, implying that the role of electron impact ionization is minor relative to photons. Auroral emission is also evident from potassium, confirming K as the major source of far red emissions seen with spacecraft imaging at Jupiter. In all cases, direct electron impact on atomic gas is sufficient to explain the brightness without invoking significant dissociative excitation of molecules. Surprisingly, the nonresponse of O and rapid depletion of Na is opposite the temporal behavior of their SO2 and NaCl parent molecules during Io’s eclipse phase.
MRI Brain Scans Classification Using Extreme Learning Machine on LBP and GLCM
Authors: Al-Awadi Jhan Yahya Rbat , Aljobouri Hadeel K. , Hasan Ali M. 
Published: February 2023

The primary goal of this study is to predict the presence of a brain tumor using MRI brain images. These images are first pre-processed to remove the boundary borders and the undesired regions. Gray-Level Co-Occurrence Matrix (GLCM) and Local Binary Pattern method (LBP) approaches are mixed for extracting multiple local and global features. The best features are selected using the ANOVA statistical approach, which is based on the largest variance. Then, the selected features are applied to many state of arts classifiers as well as to Extreme Learning Machine (ELM) neural network model, where the weights are optimized via the regularization of RELM using a suitable ratio of Cross Validation (CV) for the images' classification into one of two classes, namely normal (benign) and abnormal (malignant). The proposed ELM algorithm was trained and tested with 800 images of BRATS 2015 datasets types, and the experimental results demonstrated that this approach has better performance on several evaluation criteria, including accuracy, stability, and speedup. It reaches to 98.87% accuracy with extremely low classification time. ELM can improve the classification performance by raising the accuracy more than 2% and reducing the number of processes needed by speeding up the algorithm by a factor of 10 for an average of 20 trials.
Effect of Pawpaw Seeds on Management of Alloxan-Induced-Diabetes in Rats
Authors: Oko A.O. , Nwuzor C.C. , Ekuma Emmanuel T. 
Published: February 2023

Ethanol extract of pawpaw seed was evaluated for a possible application in the management of diabetes. Alloxan was used to induce diabetes in rats, which were subsequently used to study the antihyperglycaemic effect of the extract. Four (4) treatment groups and two (2) control groups of 8 rats each were created using complete randomized design. Triglyceride (TG), total cholesterol (TC), high density lipoprotein (HDL), low-density lipoprotein (LDL), total protein (TP), glutamic oxaloacetic transaminase (SGOT/AST), glutamic pyruvic transaminase (SGPT/ALT), alkaline phosphatase (ALP), urea and creatinine were studied using standard methods. A single dose of alloxan resulted in a significant increase (p < 0.05) in the serum TG, TC, LDL, AST, ALT, ALP, with a corresponding decrease in serum HDL, urea and creatinine. Following treatment with varying doses of the extract, there was a decrease in serum TG, TC, LDL, AST, ALT, ALP, and an increase in serum HDL, urea and creatinine. It could be inferred from the research outcome that crude extract of pawpaw seed (200 mg/kg extract) could be effective in the management of diabetes.