bluuebunny/crossref_metadata_2025_split huggingface dataset:
A Mini-Neptune Orbiting the Metal-poor K Dwarf BD+29 2654
Authors: Dai Fei , Schlaufman Kevin C. , Reggiani Henrique , Bouma Luke , Howard Andrew W. , Chontos Ashley , Pidhorodetska Daria , Van Zandt Judah , Akana Murphy Joseph M. , Rubenzahl Ryan A. , Polanski Alex S. , Lubin Jack , Beard Corey , Giacalone Steven , Holcomb Rae , Batalha Natalie M. , Crossfield Ian , Dressing Courtney , Fulton Benjamin , Huber Daniel , Isaacson Howard , Kane Stephen R. , Petigura Erik A. , Robertson Paul , Weiss Lauren M. , Belinski Alexander A. , Boyle Andrew W. , Burke Christopher J. , Castro-González Amadeo , Ciardi David R. , Daylan Tansu , Fukui Akihiko , Gill Holden , Guerrero Natalia M. , Hellier Coel , Howell Steve B. , Lillo-Box Jorge , Murgas Felipe , Narita Norio , Pallé Enric , Rodriguez David R. , Savel Arjun B. , Shporer Avi , Stassun Keivan G. , Striegel Stephanie , Caldwell Douglas A. , Jenkins Jon M. , Ricker George R. , Seager Sara , Vanderspek Roland , Winn Joshua N. 
Published: July 2023

Abstract
We report the discovery and Doppler mass measurement of a 7.4 days 2.3 R
⊕ mini-Neptune around a metal-poor K dwarf BD+29 2654 (TOI-2018). Based on a high-resolution Keck/HIRES spectrum, the Gaia parallax, and multiwavelength photometry from the UV to the mid-infrared, we found that the host star has

T

eff

=

4174

−
42

+
34

K,

log
g
=

4.62

−
0.03

+
0.02

, [Fe/H] = − 0.58 ± 0.18, M
* = 0.57 ± 0.02 M
⊙, and R
* = 0.62 ± 0.01 R
⊙. Precise Doppler measurements with Keck/HIRES revealed a planetary mass of M
p = 9.2 ± 2.1 M
⊕ for TOI-2018 b. TOI-2018 b has a mass and radius that are consistent with an Earthlike core, with a ∼1%-by-mass hydrogen/helium envelope or an ice–rock mixture. The mass of TOI-2018 b is close to the threshold for runaway accretion and hence giant planet formation. Such a threshold is predicted to be around 10M
⊕ or lower for a low-metallicity (low-opacity) environment. If TOI-2018 b is a planetary core that failed to undergo runaway accretion, it may underline the reason why giant planets are rare around low-metallicity host stars (one possibility is their shorter disk lifetimes). With a K-band magnitude of 7.1, TOI-2018 b may be a suitable target for transmission spectroscopy with the James Webb Space Telescope. The system is also amenable to metastable Helium observation; the detection of a Helium exosphere would help distinguish between a H/He-enveloped planet and a water world.
A Hydrodynamic Study of the Escape of Metal Species and Excited Hydrogen from the Atmosphere of the Hot Jupiter WASP-121b
Authors: Huang 黄 Chenliang 辰亮 , Koskinen Tommi , Lavvas Panayotis , Fossati Luca 
Published: July 2023

Abstract
In the near-UV and optical transmission spectrum of the hot Jupiter WASP-121b, recent observations have detected strong absorption features of Mg, Fe, Ca, and Hα, extending outside of the planet’s Roche lobe. Studying these atomic signatures can directly trace the escaping atmosphere and constrain the energy balance of the upper atmosphere. To understand these features, we introduce a detailed forward model by expanding the capability of a one-dimensional model of the upper atmosphere and hydrodynamic escape to include important processes of atomic metal species. The hydrodynamic model is coupled to a Lyα Monte Carlo radiative transfer calculation to simulate the excited hydrogen population and associated heating/ionization effects. Using this model, we interpret the detected atomic features in the transmission spectrum of WASP-121b and explore the impact of metals and excited hydrogen on its upper atmosphere. We demonstrate the use of multiple absorption lines to impose stronger constraints on the properties of the upper atmosphere than the analysis of a single transmission feature can provide. In addition, the model shows that line broadening due to atmospheric outflow driven by Roche lobe overflow is necessary to explain the observed line widths and highlights the importance of the high mass-loss rate caused by Roche lobe overflow, which requires careful consideration of the structure of the lower and middle atmosphere. We also show that metal species and excited-state hydrogen can play an important role in the thermal and ionization balance of ultrahot Jupiter thermospheres.
ODIN: Where Do Lyα Blobs Live? Contextualizing Blob Environments within Large-scale Structure
Authors: Ramakrishnan Vandana , Moon Byeongha , Im Sang Hyeok , Farooq Rameen , Lee Kyoung-Soo , Gawiser Eric , Yang Yujin , Park Changbom , Hwang Ho Seong , Valdes Francisco , Artale Maria Celeste , Ciardullo Robin , Dey Arjun , Gronwall Caryl , Guaita Lucia , Jeong Woong-Seob , Padilla Nelson , Singh Akriti , Zabludoff Ann 
Published: July 2023

Abstract
While many Lyα blobs (LABs) are found in and around several well-known protoclusters at high redshift, how they trace the underlying large-scale structure is still poorly understood. In this work, we utilize 5352 Lyα emitters (LAEs) and 129 LABs at z = 3.1 identified over a ∼9.5 deg2 area in early data from the ongoing One-hundred-deg2 DECam Imaging in Narrowbands (ODIN) survey to investigate this question. Using LAEs as tracers of the underlying matter distribution, we identify overdense structures as galaxy groups, protoclusters, and filaments of the cosmic web. We find that LABs preferentially reside in regions of higher-than-average density and are located in closer proximity to overdense structures, which represent the sites of protoclusters and their substructures. Moreover, protoclusters hosting one or more LABs tend to have a higher descendant mass than those which do not. Blobs are also strongly associated with filaments of the cosmic web, with ∼70% of the population being within a projected distance of ∼2.4 pMpc from a filament. We show that the proximity of LABs to protoclusters is naturally explained by their association with filaments as large cosmic structures are where many filaments converge. The contiguous wide-field coverage of the ODIN survey allows us to establish firmly a connection between LABs as a population and filaments of the cosmic web for the first time.
Photochemical Hazes Dramatically Alter Temperature Structure and Atmospheric Circulation in 3D Simulations of Hot Jupiters
Authors: Steinrueck Maria E. , Koskinen Tommi , Lavvas Panayotis , Parmentier Vivien , Zieba Sebastian , Tan Xianyu , Zhang Xi , Kreidberg Laura 
Published: July 2023

Abstract
Photochemical hazes are expected to form in hot Jupiter atmospheres and may explain the strong scattering slopes and muted spectral features observed in the transmission spectra of many hot Jupiters. Absorption and scattering by photochemical hazes have the potential to drastically alter temperature structure and atmospheric circulation of these planets but have previously been neglected in general circulation models (GCMs). We present GCM simulations of the hot Jupiter HD 189733 b that include photochemical hazes as a radiatively active tracer fully coupled to atmospheric dynamics. The influence of haze radiative feedback strongly depends on the assumed haze optical properties. For soot hazes, two distinct thermal inversions form, separated by a local temperature minimum around 10−5 bar caused by upwelling on the dayside mixing air with low haze abundance upwards. The equatorial jet broadens and slows down. The horizontal distribution of hazes remains relatively similar to simulations with radiatively passive tracers. For Titan-type hazes, the equatorial jet accelerates and extends to much lower pressures, resulting in a dramatically different 3D distribution of hazes compared to radiatively passive or soot hazes. Further experimental and observational studies to constrain the optical properties of photochemical hazes will therefore be crucial for understanding the role of hazes in exoplanetary atmospheres. In the dayside emission spectrum, for both types of hazes the amplitude of near-infrared features is reduced, while the emitted flux at longer wavelengths (>4 μm) increases. Haze radiative feedback leads to increased phase-curve amplitudes in many infrared wavelength regions, mostly due to stronger dayside emission.
Transverse Vertical Oscillations During the Contraction and Expansion of Coronal Loops
Authors: Zhang Qingmin , Zhou Yuhao , Li Chuan , Li Qiao , Xia Fanxiaoyu , Qiu Ye , Dai Jun , Zhang Yanjie 
Published: July 2023

Abstract
In this paper, we carry out a detailed analysis of the M1.6 class eruptive flare occurring in NOAA active region 13078 on 2022 August 19. The flare is associated with a fast coronal mass ejection (CME) propagating in the southwest direction with an apparent speed of ∼926 km s−1. Meanwhile, a shock wave is driven by the CME at the flank. The eruption of the CME generates an extreme-ultraviolet (EUV) wave expanding outward from the flare site with an apparent speed of ≥200 km s−1. As the EUV wave propagates eastward, it encounters and interacts with the low-lying adjacent coronal loops (ACLs), which are composed of two loops. The compression of the EUV wave results in contraction, expansion, and transverse vertical oscillations of ACLs. The commencements of contraction are sequential from western to eastern footpoints and the contraction lasts for ∼15 minutes. The speeds of contraction lie in the range of 13–40 km s−1 in 171 Å and 8–54 km s−1 in 193 Å. A long, gradual expansion follows the contraction at lower speeds. Concurrent vertical oscillations are superposed on the contraction and expansion of ACLs. The oscillations last for two to nine cycles and the amplitudes are ≤4 Mm. The periods are between 3 and 12 minutes with an average value of 6.7 minutes. The results show rich dynamics of coronal loops.
New Near-infrared Period–Luminosity–Metallicity Relations for Galactic RR Lyrae Stars Based on Gaia EDR3 Parallaxes
Authors: Zgirski Bartłomiej , Pietrzyński Grzegorz , Górski Marek , Gieren Wolfgang , Wielgórski Piotr , Karczmarek Paulina , Hajdu Gergely , Lewis Megan , Chini Rolf , Graczyk Dariusz , Kałuszyński Mikołaj , Narloch Weronika , Pilecki Bogumił , García Gonzalo Rojas , Suchomska Ksenia , Taormina Mónica 
Published: July 2023

Abstract
We present new period–luminosity and period–luminosity–metallicity relations for Galactic RR Lyrae stars based on a sample of 28 pulsators located at distances of up to 1.5 kpc from the Sun. Near-infrared photometry was obtained at the Cerro Armazones Observatory, and parallaxes were taken from the Gaia Early Data Release 3. Relations were determined for the 2MASS JHK

s
bands and the W

JK
Wesenheit index. We compare our results with other calibrations available in the literature and obtain very good agreement with the photometry of RR Lyraes from the Large Magellanic Cloud (LMC) anchored using the distance to the Cloud, which is based on detached eclipsing binaries. We find that the dependence of absolute magnitudes on metallicity of 0.070 ± 0.042 (J band) to 0.087 ± 0.031 (W

JK
index) mag dex−1 for the population of fundamental pulsators (RRab) is in agreement with previously published phenomenological works. We perform a refined determination of distance to the LMC based on our new calibration and photometry from Szewczyk et al. We study the dependence of the fitted parameters of the fiducial relations and the LMC distance on the systematic parallax offset.
Core-collapse Supernova Simulations with Reduced Nucleosynthesis Networks
Authors: Navó Gerard , Reichert Moritz , Obergaulinger Martin , Arcones Almudena 
Published: July 2023

Abstract
We present core-collapse supernova simulations including nuclear reaction networks that impact explosion dynamics and nucleosynthesis. The different composition treatment can lead to changes in the neutrino heating in the vicinity of the shock by modifying the number of nucleons and thus the neutrino-opacity of the region. This reduces the ram pressure outside the shock and allows an easier expansion. The energy released by the nuclear reactions during collapse also slows down the accretion and aids the shock expansion. In addition, nuclear energy generation in the postshocked matter produces up to 20% more energetic explosions. Nucleosynthesis is affected due to the different dynamic evolution of the explosion. Our results indicate that the energy generation from nuclear reactions helps to sustain late outflows from the vicinity of the proto-neutron star, synthesizing more neutron-rich species. Furthermore, we show that there are systematic discrepancies between the ejecta calculated with in situ and ex situ reaction networks. These differences stem from the intrinsic characteristics of evolving the composition in hydrodynamic simulations or calculating it with Lagrangian tracer particles. The mass fractions of some Ca, Ti, Cr, and Fe isotopes are consistently underproduced in postprocessing calculations, leading to different nucleosynthesis paths. Our results suggest that large in situ nuclear reaction networks are important for a realistic feedback of the energy generation, the neutrino heating, and a more accurate ejecta composition.
Aluminium-26 from Massive Binary Stars. III. Binary Stars up to Core Collapse and Their Impact on the Early Solar System
Authors: Brinkman Hannah E. , Doherty Carolyn , Pignatari Marco , Pols Onno , Lugaro Maria 
Published: July 2023

Abstract
Many of the short-lived radioactive nuclei that were present in the early solar system can be produced in massive stars. In the first paper in this series, we focused on the production of 26Al in massive binaries. In our second paper, we considered rotating single stars; two more short-lived radioactive nuclei, 36Cl and 41Ca; and the comparison to the early solar system data. In this work, we update our previous conclusions by further considering the impact of binary interactions. We used the MESA stellar evolution code with an extended nuclear network to compute massive (10–80 M
⊙), binary stars at various initial periods and solar metallicity (Z = 0.014), up to the onset of core collapse. The early solar system abundances of 26Al and 41Ca can be matched self-consistently by models with initial masses ≥25 M
⊙, while models with initial primary masses ≥35 M
⊙ can also match 36Cl. Almost none of the models provide positive net yields for 19F, while for 22Ne the net yields are positive from 30 M
⊙ and higher. This leads to an increase by a factor of approximately 4 in the amount of 22Ne produced by a stellar population of binary stars, relative to single stars. In addition, besides the impact on the stellar yields, our 10 M
⊙ primary star undergoing Case A mass transfer ends its life as a white dwarf instead of as a core-collapse supernova. This demonstrates that binary interactions can also strongly impact the evolution of stars close to the supernova boundary.
MASTER OT J030227.28+191754.5: A Dwarf Nova at a Massive Oxygen–Neon White Dwarf System?
Authors: Kimura Mariko , Kashiyama Kazumi , Shigeyama Toshikazu , Tampo Yusuke , Yamada Shinya , Enoto Teruaki 
Published: July 2023

Abstract
We present timing and spectral analysis results of the NICER and NuSTAR observations of the dwarf nova MASTER OT J030227.28+191754.5 during the 2021–2022 outburst. The soft X-ray component was found to be dominated by blackbody radiation with a temperature of ∼30 eV and also showed prominent oxygen and neon emission lines. The blackbody luminosity exceeded 1034 erg s−1, which is consistent with theoretical predictions, and then decreased more than an order of magnitude in 3.5 days. The inferred abundances of oxygen and neon in the optically thin coronal region surrounding the central white dwarf (WD) are several times higher than the respective solar values. Although inconclusive, the abundance enrichment may originate from the WD, indicating that it may be mainly composed of oxygen and neon. Assuming that the blackbody radiation comes from the belt-shaped boundary layer between the WD and the accretion disk, we estimated the WD radius to be (2.9 ± 1.1) × 108 cm, which corresponds to the WD mass range of 1.15–1.34 M
⊙. If the accretion continues for another ∼1 Gyr, the WD may experience an accretion-induced collapse into a neutron star and form a so-called black widow pulsar system.
The NANOGrav 12.5 yr Data Set: Bayesian Limits on Gravitational Waves from Individual Supermassive Black Hole Binaries
Authors: Arzoumanian Zaven , Baker Paul T. , Blecha Laura , Blumer Harsha , Brazier Adam , Brook Paul R. , Burke-Spolaor Sarah , Bécsy Bence , Casey-Clyde J. Andrew , Charisi Maria , Chatterjee Shami , Chen Siyuan , Cordes James M. , Cornish Neil J. , Crawford Fronefield , Cromartie H. Thankful , DeCesar Megan E. , Demorest Paul B. , Dolch Timothy , Drachler Brendan , Ellis Justin A. , Ferrara E. C. , Fiore William , Fonseca Emmanuel , Freedman Gabriel E. , Garver-Daniels Nathan , Gentile Peter A. , Glaser Joseph , Good Deborah C. , Gültekin Kayhan , Hazboun Jeffrey S. , Jennings Ross J. , Johnson Aaron D. , Jones Megan L. , Kaiser Andrew R. , Kaplan David L. , Kelley Luke Zoltan , Key Joey Shapiro , Laal Nima , Lam Michael T. , Lamb William G , W. Lazio T. Joseph , Lewandowska Natalia , Liu Tingting , Lorimer Duncan R. , Luo Jing , Lynch Ryan S. , Madison Dustin R. , McEwen Alexander , McLaughlin Maura A. , Mingarelli Chiara M. F. , Ng Cherry , Nice David J. , Ocker Stella Koch , Olum Ken D. , Pennucci Timothy T. , Pol Nihan S. , Ransom Scott M. , Ray Paul S. , Romano Joseph D. , Shapiro-Albert Brent J. , Siemens Xavier , Simon Joseph , Siwek Magdalena , Spiewak Renée , Stairs Ingrid H. , Stinebring Daniel R. , Stovall Kevin , Swiggum Joseph K. , Sydnor Jessica , Taylor Stephen R. , Turner Jacob E. , Vallisneri Michele , Vigeland Sarah J. , Wahl Haley M. , Walsh Gregory , Witt Caitlin A. , Young Olivia ,   The NANOGrav Collaboration
Published: July 2023

Abstract
Pulsar timing array collaborations, such as the North American Nanohertz Observatory for Gravitational Waves (NANOGrav), are seeking to detect nanohertz gravitational waves emitted by supermassive black hole binaries formed in the aftermath of galaxy mergers. We have searched for continuous waves from individual circular supermassive black hole binaries using NANOGrav’s recent 12.5 yr data set. We created new methods to accurately model the uncertainties on pulsar distances in our analysis, and we implemented new techniques to account for a common red-noise process in pulsar timing array data sets while searching for deterministic gravitational wave signals, including continuous waves. As we found no evidence for continuous waves in our data, we placed 95% upper limits on the strain amplitude of continuous waves emitted by these sources. At our most sensitive frequency of 7.65 nHz, we placed a sky-averaged limit of h
0 < (6.82 ± 0.35) × 10−15, and h
0 < (2.66 ± 0.15) × 10−15 in our most sensitive sky location. Finally, we placed a multimessenger limit of


<
(
1.41
±
0.02
)
×

10
9

M
⊙

on the chirp mass of the supermassive black hole binary candidate 3C 66B.
Investigating Possible Binarity for GJ 229B
Authors: Howe Alex R. , Mandell Avi M. , McElwain Michael W. 
Published: July 2023

Abstract
GJ 229B, the first type-T brown dwarf to be discovered, has presented a tension between comparisons with evolutionary models and the larger-than-expected mass and radius values derived from spectroscopic and astrometric observations. We examine the hypothesis that GJ 229B is actually a binary substellar object by using two grid-based fits using evolutionary models to explore the range of mass ratios of the possible binary components. We find that the best-fit component values are most consistent with a roughly 2:1 binary mass ratio and an age range of 2–6 Gyr. The observed temperatures, masses, and apparent radii match expected values from evolutionary models for a binary much better than a single-object model, but more detailed observations and modeling are needed to definitively confirm the binary hypothesis.
Trends in Collegiate Student-Athlete Mental Health in the National College Health Assessment, 2011–2019
Authors: Edwards Brian , Froehle Andrew W. , Fagan Siobhan E. 
Published: July 2023

Context
Recently, the athletic training community has paid increased attention to collegiate student-athlete mental health, mental health treatment-seeking behavior, and the effects of mental health factors on athletic and academic performance. Ongoing efforts to better educate and equip athletic trainers to help student-athletes in this regard should result in improved mental health–related outcomes.

Objective
To examine changes in the mental health of student-athletes over the past decade compared with that of nonathlete students.

Design
Cross-sectional study.

Setting
Colleges and universities in the United States.

Patients or Other Participants
Varsity athletes (athletes; n = 54 479) and nonathlete students (nonathletes; n = 448 301) who completed the National College Health Assessment between 2011 and 2019.

Main Outcome Measure(s)
Surveys included responses (self-reported) to questions in 5 mental health–related categories: recent mental health symptoms, recent mental health diagnosis, mental health treatment-seeking behavior, receiving mental health information from the institution, and the recent effect of mental health factors on academic performance.

Results
Athletes consistently described lower symptom and diagnosis rates compared with nonathletes, except for attempted suicide, substance abuse, and eating disorders. Rates of diagnosis increased over time in both groups but remained lower in athletes. Treatment-seeking behavior and openness to future treatment increased over time in both groups but remained lower in athletes. Athletes received more information on stress reduction, substance abuse, eating disorders, and handling distress or violence compared with nonathletes. Both groups received information more frequently over time. Athletes reported fewer academic effects, especially for depression and anxiety, but these effects grew over time in both groups. The effects of injuries and extracurricular activities on academic performance were greater in athletes than in nonathletes.

Conclusions
Athletes described overall lower levels of mental health symptoms, diagnoses, and academic effects compared with nonathletes. Whereas the rates in nonathletes climbed over the past decade, the rates in athletes broadly remained flat or climbed less rapidly. Increasingly positive attitudes toward treatment were encouraging, but the deficit in athletes relative to nonathletes persisted. Ongoing efforts of athletic trainers to educate athletes and guide them to mental health resources are needed to continue, or better yet to accelerate, the observed positive trends in information dissemination and treatment-seeking behavior.