bluuebunny/crossref_metadata_2025 huggingface dataset:
Environmental Health Perspectives on the Emergence and Re-Emergence of Infectious Diseases, Geopolitics and Gain of Function Research
Authors: SR Chrysanthus Chukwuma
Published: January 2022

Research and publication are relevant from perspectives in the management of local and global health because disease is perspicuously a geopolitical issue ostensibly linked to gain-of-function research where health diplomacy undergirds present and future global functionalities regarding the emergence and reemergence of infectious diseases. These have generated vehement reactions with propensity for extreme geopolitics and gain-of-function natural and anthropogenic activities. Geopolitical parameters and gain-of-function issues impact on the social determinants of health and vice versa. The convening and convergence of countries for unprecedented epidemic or pandemic treaty settings or other formulations to confront emerging and reemerging infectious diseases will afford considerable opportunities concerning challenges in action, preparedness and response. Provisions are pertinent for legal instruments, effective and efficient systems to curb future threats and outbreaks of infectious diseases.
Kutatói aranybánya? A Modus Operandi Nyilvántartás kutathatósága
Authors: Baráth Emőke Noémi
Published: January 2022

The study presents the research potential of a criminal record system that often appears abroad in the criminal psychology literature. The study undertakes to explore the possibilities of the Hungarian Modus Operandi Register that can be used in research, with a special focus on what data are available and how their analysis could contribute to the development of criminal profiling. Foreign examples show that research in the Modus Operandi Register has yielded important results in identifying types of homicides and preventing victimization of sexual offenses, as well as in sexual homicides against children. The article processed domestic and foreign literature and research results. The main consideration was to summarize the results obtained using the data from the Modus Operandi Register. Modus Operandi can indeed be a research treasure trove if access to data – in compliance with the legal framework – allows researchers to carry out analyses, and if the incorporation of their findings is encouraged by the law enforcement officials. Another area of research could be to analyse patterns of criminal careers, as well as to examine what kind of criminal diversity can be discovered for each offender and how this affects his or her methods. Finally, it could be examined to what extent the trends that can be discovered in international research appear among Hungarian criminals. These approaches may contribute to a more efficient operation of the police.
Egy kábítószer készítésének elősegítése bűntett nyomozása és tanulságai
Authors: Hertelendi Lajos
Published: January 2022

False preparations are not produced in laboratories but especially in the form of „DIY” under far not sterile conditions. Pills, produced in generally in sheds, will be coated in concrete mixers and dried laid on the floor. The agents will be replaced by useless and for human consumption unsuitable materials. By inspection of false preparations were already found chalk powder, drugs, and in coloured products, brick-dust used as filling material. It is a well-known fact, that the most drugs, suspicious or false drug deliveries arrive from Far East countries but the knowledge of the country of dispatch alone does not necessarily result in opening of a small consignment or even of a big cargo by the National Tax and Customs Administration. A risk analyse is made, checking many features before opening a package, as only in this way they can process thousands of packages a day. In this paper we present the liquidation of a criminal gang in Hungary, whose members made their names memorable in the law enforcement ledger by production and distribution of desire and performance enhancers.
Hogyan döntünk? …és hogyan kellene?
Authors: Németh Viktor
Published: January 2022

Jonah Lehrer’s book examines and presents decision-making processes through practical examples. The essential questions of the book are the following: ‘How is the human mind deciding? And how can I improve these decisions?’ (Lehrer, 2012). Decision-making mechanisms define our everyday lives. This is valid for our workplace as well as for our private life too. Scientists believe in the rational brain for centuries. In various disciplines, unanimous decisions based on sheer rationality alone is considered to be correct and acceptable. The book of Lehrer gives a much more sophisticated picture of the decision-making mechanism of the human brain. Enlightening that some brain areas developed during evolution, how they contribute to each decision-making processes. Practical examples illustrate the relationship between emotions and rationality during decision-making.
A kiberbűncselekmények felderítésének nehézségei
Authors: Herédi István
Published: January 2022

One of the current challenges law enforcement agencies are facing, is ensuring the effective and proactive fight against cybercrime. This category of crime is characterized by its latent nature and detection difficulties that can significantly slow down the prosecution process or even make it impossible for the law enforcement agencies to conduct successful investigations. With the growing of the number of the active internet-users, new interfaces and services are emerging in the online space, which also creates opportunities for the rise of new types of crime. In general, cybersecurity threats are on the rise. The anonymity provided by cyberspace acts as an incentive for offenders, as they are much less likely to be caught as if they were committing a contactbased crime, and the damage caused is much greater if we are speaking about cybercrime affecting assets. Detection difficulties do not depend on the complexity/seriousness of the cybercrime. Simple cyber-enabled crime is just as difficult to uncover as sophisticated cyber-attacks. The main difficulties are related to the use of online identity masking services, technical innovation and gaps in international cooperation among authorities. Possible solutions can offer the use of direct international cooperation, in particular 24/7 (always available) contact networks, the active use of opensource investigations and online profiling, and the regular training of law enforcement personnel. If the specific issue at stake is beyond the knowledge of the intelligence services’ staff, it may be appropriate to involve specialized advisers or experts with specific expertise.
A hálózatelemzés elmélete és rendőrségi gyakorlata
Authors: Keszi Tamás , Lohner Klaudia
Published: January 2022

The aim of our study is to highlight the usefulness of network analysis methods in the field of law enforcement, and that the future of this field depends on collaboration and productive cooperation of theory and practice. After a brief historical overview, we introduce the most important concepts related to network analysis and graph theory, and then present a possible resolution strategy for a mafia network. Finally, we provide an overview of the directions of network analysis that can be used in profiling.
A rendőri jogalkalmazás társadalmi értékelésének netnográfiai vizsgálata
Authors: Christián László , Erdős Ákos
Published: January 2022

Netnography is an adaptable, fast and efficient, qualitative research method that uses public online spaces as data source to identify and understand the culture, mindset, decision-making mechanisms (Dörnyei & Mitev, 2010b) and attitudes of the rapidly evolving and disintegrating internet user groups. Netnography research method used in our study provides a novel opportunity to study social attitudes of law enforcement and police officers, as well as internet users’ opinions about the authority and its members. In this study, we systematically analyse the online discourse around an event occured in May 2020 in Budapest. Our results suggest that online community platforms rarely provide objective assessments of law enforcement and social evaluation of the police authority (6,73%). In a significant proportion of the opinions (58,35%), the facts related to the specific act published in the media do not actually play a decisive role. The majority of contributors are clearly biased towards either the individual subject to police measures or the acting authority. Those in the so-called critical sub-dimension, who have negative perception towards the applied measures or the police, makes up nearly the one fifth (18,13%) of the total number of items. The proportion of respondents in the supportive sub-dimension (12,08%) is slightly lower. Based on the results, it can be stated with a high degree of certainty that the attitude towards the police or law enforcement cannot be significantly influenced by a single press report, neither in positive nor in negative direction.
A feljelentési hajlandóság és a rendőrségbe vetett bizalom összefüggései. Szisztematikus szakirodalmi áttekintés a Web of Science alapján
Authors: Füstös Mónika
Published: January 2022

For many years criminology has assumed that the more victims trust the police, the more they will be willing to report crimes. Yet, the relationship between trust in the police and victims’ willingness to report has rarely been considered empirically. In the last few years, however, the topic has been attracting more and more attention worldwide. This study reviews the articles published on this topic in English so far and examines them from the perspective of scientific metrics, including the numerical distribution of the correlation. Using the search function of Web of Science, a total of 41 articles were found published between 1975 and 2020 that studied the relationship between the two concepts. Analysing these, it has emerged that research interest in the subject has increased over the past five years, primarily in criminology, but also in the fields of law and social sciences. The results also show that most researches comes from economically more developed regions, mainly Anglo-Saxon areas. The main finding of this article is that the research results are inconsistent. Although most researches confirms the relationship between trust in the police and willingness to report crimes, there are many studies that contradict this. Furthermore, the controversial results do not seem to correlate with the level of economic development nor with the date when the research was published. Therefore, the relationship between trust in the police and the willingness to report crimes should also be researched using qualitative methods in order to gain a deeper understanding of this complex topic, and questionnaires should be designed specifically for this purpose.
CASE STUDY ON PERFORMANCE MONITORING AND STABILITY ANALYSIS OF BAISHIHU SUSPENSION BRIDGE AND SIDE SLOPE
Authors: Chen Chihcheng , Shih Ban-Jwu , Jeng Ching-Jiang
Published: January 2022

The main structure of the Baishihu suspension bridge was connected to the anchor foundations by three main steel cables. The wooden pedestrian deck was fixed to the main steel cables using steel beams and was stabilized by two stabilizing cables. The stabilizing cables and bridge body were joined by 44 steel connecting rods. Therefore, the slope stability at the anchorage foundations of the main steel cables, as well as the performance monitoring and analysis of the main steel cables and stabilizing cables, are critical to the overall performance of the suspension bridge. This paper discusses the performance monitoring and analysis of the steel cable deflection and cable strength for this bridge, as well as the main considerations and results of the stability analysis of the bridge abutments and side slopes of the two banks. Water-level observation wells, inclinometers, and tiltmeters monitoring were used to record reference data for the analysis of the slope stability performance. Additionally, the three-dimensional dynamic analysis program VFIFE was used to analyze the deformation and motion of the bridge. The final steady-state results were used to compare the static design value and monitoring data. The dynamic response before the final steady state was also observed.
Dynamical Mass of the Young Substellar Companion HD 984 B
Authors: Franson Kyle , Bowler Brendan P. , Brandt Timothy D. , Dupuy Trent J. , Tran Quang H. , Brandt G. Mirek , Li Yiting , Kraus Adam L.
Published: January 2022

Model-independent masses of substellar companions are critical tools to validate models of planet and brown dwarf cooling, test their input physics, and determine the formation and evolution of these objects. In this work, we measure the dynamical mass and orbit of the young substellar companion HD 984 B. We obtained new high-contrast imaging of the HD 984 system with Keck/NIRC2 that expands the baseline of relative astrometry from 3 to 8 yr. We also present new radial velocities of the host star with the Habitable-Zone Planet Finder spectrograph at the Hobby-Eberly Telescope. Furthermore, HD 984 exhibits a significant proper motion difference between Hipparcos and Gaia EDR3. Our joint orbit fit of the relative astrometry, proper motions, and radial velocities yields a dynamical mass of 61 ± 4 M
Jup for HD 984 B, placing the companion firmly in the brown dwarf regime. The new fit also reveals a higher eccentricity for the companion (e = 0.76 ± 0.05) compared to previous orbit fits. Given the broad age constraint for HD 984, this mass is consistent with predictions from evolutionary models. HD 984 B’s dynamical mass places it among a small but growing list of giant planet and brown dwarf companions with direct mass measurements.
Investigating the Baryon Cycle in Interacting Dwarfs with the Very Large Array and Pan-STARRS
Authors: Luber N. , Pearson Sarah , Putman Mary E. , Besla Gurtina , Stierwalt Sabrina , Meyers Joel P.
Published: January 2022

We present resolved H i synthesis maps from the Very Large Array of three interacting dwarf systems: the NGC 3664 dwarf pair, the NGC 3264 dwarf pair, and the UGC 4638 dwarf triplet. All three dwarf systems are captured at various stages of interaction and span a range of environments. We detect clear hallmarks of tidal interactions through the presence of H i bridges and diffuse H i extensions that surround the dwarfs. We overlay the H i data on Pan-STARRS r-band images and find further evidence of tidal interactions through coincident distorted H i and tidal stellar features in NGC 3264 and UGC 4638, and an unwound spiral arm pointing toward its smaller companion in NGC 3264. In UGC 4638, both the gas and diffuse stars are extended to similar radii east of the primary, which could indicate that the smaller dwarf in the system has already completed one pass through the primary. We additionally find that our three systems, and those from the Local Volume TiNy Titans survey, are not H i deficient and thus the interaction has not resulted in a loss of gas from the systems. A comparison with noninteracting dwarf galaxies shows that the interactions have a significant impact on the kinematics of the systems. Our new resolved H i kinematics, combined with detailed stellar and H i morphologies, provide crucial constraints for future dynamical modeling of hierarchical mergers and the baryon cycle at the low-mass scale.
TESS Giants Transiting Giants. I.: A Noninflated Hot Jupiter Orbiting a Massive Subgiant
Authors: Saunders Nicholas , Grunblatt Samuel K. , Huber Daniel , Collins Karen A. , Jensen Eric L. N. , Vanderburg Andrew , Brahm Rafael , Jordán Andrés , Espinoza Néstor , Henning Thomas , Hobson Melissa J. , Quinn Samuel N. , Zhou George , Butler R. Paul , Crause Lisa , Kuhn Rudi B. , Moses Mogotsi K. , Hellier Coel , Angus Ruth , Hattori Soichiro , Chontos Ashley , Ricker George R. , Jenkins Jon M. , Tenenbaum Peter , Latham David W. , Seager Sara , Vanderspek Roland K. , Winn Joshua N. , Stockdale Chris , Cloutier Ryan
Published: January 2022

While the population of confirmed exoplanets continues to grow, the sample of confirmed transiting planets around evolved stars is still limited. We present the discovery and confirmation of a hot Jupiter orbiting TOI-2184 (TIC 176956893), a massive evolved subgiant (M
⋆ = 1.53 ± 0.12 M
⊙, R
⋆ = 2.90 ± 0.14 R
⊙) in the Transiting Exoplanet Survey Satellite (TESS) Southern Continuous Viewing Zone. The planet was flagged as a false positive by the TESS Quick-Look Pipeline due to periodic systematics introducing a spurious depth difference between even and odd transits. Using a new pipeline to remove background scattered light in TESS Full Frame Image data, we combine space-based TESS photometry, ground-based photometry, and ground-based radial velocity measurements to report a planet radius of R

p
= 1.017 ± 0.051 R

J
and mass of M

p
= 0.65 ± 0.16 M

J
. For a planet so close to its star, the mass and radius of TOI-2184b are unusually well matched to those of Jupiter. We find that the radius of TOI-2184b is smaller than theoretically predicted based on its mass and incident flux, providing a valuable new constraint on the timescale of post-main-sequence planet inflation. The discovery of TOI-2184b demonstrates the feasibility of detecting planets around faint (TESS magnitude > 12) post-main-sequence stars and suggests that many more similar systems are waiting to be detected in the TESS FFIs, whose confirmation may elucidate the final stages of planetary system evolution.
Unbound Close Stellar Encounters in the Solar Neighborhood
Authors: Hansen Bradley M. S.
Published: January 2022

We present a catalog of unbound stellar pairs, within 100 pc of the Sun, that are undergoing close, hyperbolic, encounters. The data are drawn from the GAIA EDR3 catalog, and the limiting factors are errors in the radial distance and unknown velocities along the line of sight. Such stellar pairs have been suggested to be possible events associated with the migration of technological civilizations between stars. As such, this sample may represent a finite set of targets for a SETI search based on this hypothesis. Our catalog contains a total of 132 close passage events, featuring stars from across the entire main sequence, with 16 pairs featuring at least one main-sequence star of spectral type between K1 and F3. Many of these stars are also in binaries, so that we isolate eight single stars as the most likely candidates to search for an ongoing migration event—HD 87978, HD 92577, HD 50669, HD 44006, HD 80790, LSPM J2126+5338, LSPM J0646+1829 and HD 192486. Among host stars of known planets, the stars GJ 433 and HR 858 are the best candidates.
The Effect of Post-Newtonian Spin Precessions on the Evolution of Exomoons’ Obliquity
Authors: Iorio Lorenzo
Published: January 2022

Putative natural massive satellites (exomoons) have gained increasing attention when they orbit Jupiter-like planets within the habitable zone of their host main-sequence star S. An exomoon s is expected to move within the equatorial plane of its host planet p, with its spin
S

s aligned with its orbital angular momentum
L
, which, in turn, is parallel to the planetary spin
S

p. If, in particular, the common tilt ε of such angular momenta to the plane of the satellite–planet motion about the star, assumed fixed, has certain values, the stellar latitudinal irradiation experienced on the exomoon may allow it to sustain life as we know it, at least for certain orbital configurations. An Earth analog (similar in mass, radius, oblateness, and obliquity) is considered, which orbits within 5–10 planetary radii R
p from its Jupiter-like host planet. The de Sitter and Lense–Thirring spin precessions due to the general relativistic post-Newtonian (pN) field of the host planet have an impact on an exomoon’s habitability for a variety of different initial spin–orbit configurations. Here I show it by identifying long-term variations in the satellite’s obliquity ε
s, where variations can be ≲10°–100°, depending on the initial spin–orbit configuration, with a timescale of ≃0.1–1 million years. Also the satellite’s quadrupole mass moment

J

2

s

induces obliquity variations that are faster than the pN ones but do not cancel them. Tidal dissipations, which may potentially have a relevant impact on the outlined pattern, are not included in the present analysis.
A Census of Stars and Disks in Corona Australis*
Authors: Esplin T. L. , Luhman K. L.
Published: January 2022

We have performed a census of the young stellar populations near the Corona Australis molecular cloud using photometric and kinematic data from several sources, particularly Gaia EDR3, and spectroscopy of hundreds of candidate members. We have compiled a catalog of 393 members of Corona Australis, (39 at >M6), 293 (36) of which are spectroscopically classified for the first time in this work. We find that Corona Australis can be described in terms of two stellar populations, a younger one (a few megayears) that is partially embedded in the cloud (the Coronet Cluster) and an older one (∼15 Myr) that surrounds and extends beyond the cloud (Upper Corona Australis). These populations exhibit similar space velocities, and we find no evidence for distinct kinematic populations in Corona Australis, in contrast to a recent study based on Gaia DR2. The distribution of spectral types in Corona Australis reaches a maximum at M5 (∼0.15 M
⊙), indicating that the initial mass function has a similar characteristic mass as other nearby star-forming regions. Finally, we have compiled mid-infrared photometry from the Wide-field Infrared Survey Explorer and the Spitzer Space Telescope for the members of Corona Australis, and we have used those data to identify and classify their circumstellar disks. Excesses are detected for 122 stars, one-third of which are reported for the first time in this work.
Optical Studies of 10 Hard X-Ray-selected Cataclysmic Binaries
Authors: Halpern Jules P. , Thorstensen John R.
Published: January 2022

We conducted time-resolved optical spectroscopy and/or photometry of 10 cataclysmic binaries that were discovered in hard X-ray surveys, with the goal of measuring their orbital periods and searching for evidence that they are magnetic. Four of the objects in this study are new optical identifications: IGR J18017−3542, PBC J1841.1+0138, IGR J18434−0508, and Swift J1909.3+0124. A 311.8 s, coherent optical pulsation is detected from PBC J1841.1+0138, as well as eclipses with a period of 0.221909 days. A 152.49 s coherent period is detected from IGR J18434−0508. A probable period of 389 s is seen in IGR J18151−1052, in agreement with a known X-ray spin period. We also detect a period of 803.5 s in an archival X-ray observation of Swift J0717.8−2156. The last four objects are thus confirmed magnetic cataclysmic variables of the intermediate polar class. An optical period of 1554 s in AX J1832.3−0840 also confirms the known X-ray spin period, but a stronger signal at 2303 s is present whose interpretation is not obvious. We also studied the candidate intermediate polar Swift J0820.6−2805, which has low and high states differing by ≈4 mag and optical periods or quasi-periodic oscillations not in agreement with proposed X-ray periods. Of note is an unusually long 2.06-day orbital period for Swift J1909.3+0124, manifest in the radial velocity variation of photospheric absorption lines of an early K-type companion star. The star must be somewhat evolved if it is to fill its Roche lobe.
Lyman Continuum Galaxy Candidates in COSMOS
Authors: Prichard Laura J. , Rafelski Marc , Cooke Jeff , Meštrić Uros , Bassett Robert , Ryan-Weber Emma V. , Sunnquist Ben , Alavi Anahita , Hathi Nimish , Wang Xin , Revalski Mitchell , Bajaj Varun , O’Meara John M. , Spitler Lee
Published: January 2022

Star-forming galaxies are the sources likely to have reionized the universe. As we cannot observe them directly due to the opacity of the intergalactic medium at z ≳ 5, we study z ∼ 3–5 galaxies as proxies to place observational constraints on cosmic reionization. Using new deep Hubble Space Telescope rest-frame UV F336W and F435W imaging (30 orbits, ∼40 arcmin2, ∼29–30 mag depth at 5σ), we attempt to identify a sample of Lyman continuum galaxies (LCGs). These are individual sources that emit ionizing flux below the Lyman break (<912 Å). This population would allow us to constrain cosmic reionization parameters such as the number density and escape fraction (f
esc) of ionizing sources. We compile a comprehensive parent sample that does not rely on the Lyman-break technique for redshifts. We present three new spectroscopic candidates at z ∼ 3.7–4.4 and 32 new photometric candidates. The high-resolution multiband HST imaging and new Keck/Low Resolution Imaging Spectrometer (LRIS) redshifts make these promising spectroscopic LCG candidates. Using both a traditional and a probabilistic approach, we find that the most likely f
esc values for the three spectroscopic LCG candidates are >100% and therefore not physical. We are unable to confirm the true nature of these sources with the best available imaging and direct blue Keck/LRIS spectroscopy. More spectra, especially from the new class of 30 m telescopes, will be required to build a statistical sample of LCGs to place firm observational constraints on cosmic reionization.
Flows in Enthalpy-based Thermal Evolution of Loops
Authors: Rajhans Abhishek , Tripathi Durgesh , Bradshaw Stephen J. , Kashyap Vinay L. , Klimchuk James A.
Published: January 2022

Plasma-filled loop structures are common in the solar corona. Because detailed modeling of the dynamical evolution of these structures is computationally costly, an efficient method for computing approximate but quick physics-based solutions is to rely on space-integrated 0D simulations. The enthalpy-based thermal evolution of loops (EBTEL) framework is a commonly used method to study the exchange of mass and energy between the corona and transition region. EBTEL solves for density, temperature, and pressure, averaged over the coronal part of the loop, velocity at coronal base, and the instantaneous differential emission measure distribution in the transition region. The current single-fluid version of the code, EBTEL2, assumes that at all stages the flows are subsonic. However, sometimes the solutions show the presence of supersonic flows during the impulsive phase of heat input. It is thus necessary to account for this effect. Here, we upgrade EBTEL2 to EBTEL3 by including the kinetic energy term in the Navier–Stokes equation. We compare the solutions from EBTEL3 with those obtained using EBTEL2, as well as the state-of-the-art field-aligned hydrodynamics code HYDRAD. We find that the match in pressure between EBTEL3 and HYDRAD is better than that between EBTEL2 and HYDRAD. Additionally, the velocities predicted by EBTEL3 are in close agreement with those obtained with HYDRAD when the flows are subsonic. However, EBTEL3 solutions deviate substantially from HYDRAD’s when the latter predicts supersonic flows. Using the mismatches in the solution, we propose a criterion to determine the conditions under which EBTEL can be used to study flows in the system.
Chemical Differentiation of Planets: A Core Issue
Authors: Toulhoat Hervé , Zgonnik Viacheslav
Published: January 2022

By plotting empirical chemical element abundances on Earth relative to the Sun and normalized to silicon versus their first ionization potentials, we confirm the existence of a correlation reported earlier. To explain this, we develop a model based on principles of statistical physics that predicts differentiated relative abundances for any planetary body in a solar system as a function of its orbital distance. This simple model is successfully tested against available chemical composition data from CI chondrites and surface compositional data of Mars, Earth, the Moon, Venus, and Mercury. We show, moreover, that deviations from the proposed law for a given planet correspond to later surface segregation of elements driven both by gravity and chemical reactions. We thus provide a new picture for the distribution of elements in the solar system and inside planets, with important consequences for their chemical composition. Particularly, a 4 wt% initial hydrogen content is predicted for bulk early Earth. This converges with other works suggesting that the interior of the Earth could be enriched with hydrogen.
Age Spreads and Systematics in λ Orionis with Gaia DR2 and the SPOTS Tracks
Authors: Cao Lyra , Pinsonneault Marc H. , Hillenbrand Lynne A. , Kuhn Michael A.
Published: January 2022

In this paper we investigate the robustness of age measurements, age spreads, and stellar models in young pre-main-sequence stars. For this effort, we study a young cluster, λ Orionis, within the Orion star-forming complex. We use Gaia data to derive a sample of 357 targets with spectroscopic temperatures from spectral types or from the automated spectroscopic pipeline in APOGEE Net. After accounting for systematic offsets between the spectral type and APOGEE temperature systems, the derived properties of stars on both systems are consistent. The complex interstellar medium, with variable local extinction, motivates a star-by-star dereddening approach. We use a spectral energy distribution fitting method calibrated on open clusters for the Class III stars. For the Class II population, we use a Gaia G-RP dereddening method, minimizing systematics from disks, accretion, and other physics associated with youth. The cluster age is systematically different in models incorporating the structural impact of starspots or magnetic fields than in nonmagnetic models. Our mean ages range from 2–3 Myr (nonmagnetic models) to 3.9 ± 0.2 Myr in the SPOTS model (f = 0.34). We find that star-by-star dereddening methods distinguishing between pre-main-sequence classes provide a smaller age spread than techniques using a uniform extinction, and we infer a minimum age spread of 0.19 dex and a typical age spread of 0.35 dex after modeling age distributions convolved with observed errors. This suggests that the λ Ori cluster may have a long star formation timescale and that spotted stellar models significantly change age estimates for young clusters.
Evolution of C iv Absorbers. II. Where Does C iv Live?
Authors: Hasan Farhanul , Churchill Christopher W. , Stemock Bryson , Nielsen Nikole M. , Kacprzak Glenn G. , Croom Mark , Murphy Michael T.
Published: January 2022

We use the observed cumulative statistics of C iv absorbers and dark matter halos to infer the distribution of C iv-absorbing gas relative to galaxies at redshifts 0 ≤ z ≤ 5. We compare the cosmic incidence dN/dX of C iv absorber populations and galaxy halos, finding that massive L ≥ L
⋆ halos alone cannot account for all the observed W

r
≥ 0.05 Å absorbers. However, the dN/dX of lower-mass halos exceeds that of W

r
≥ 0.05 Å absorbers. We also estimate the characteristic gas radius of absorbing structures required for the observed C iv
dN/dX, assuming each absorber is associated with a single galaxy halo. The W

r
≥ 0.3 Å and W

r
≥ 0.6 Å C iv gas radii are ∼30%–70% (∼20%–40%) of the virial radius of L
⋆ (0.1L
⋆) galaxies, and the W

r
≥ 0.05 Å gas radius is ∼100%–150% (∼60%–100%) of the virial radius of L
⋆ (0.1L
⋆) galaxies. For stronger absorbers, the gas radius relative to the virial radius rises across Cosmic Noon and falls afterwards, while for weaker absorbers, the relative gas radius declines across Cosmic Noon and then dramatically rises at z < 1. A strong luminosity-dependence of the gas radius implies highly extended C iv envelopes around massive galaxies before Cosmic Noon, while a luminosity-independent gas radius implies highly extended envelopes around dwarf galaxies after Cosmic Noon. From available absorber-galaxy and C iv evolution data, we favor a scenario in which low-mass galaxies enrich the volume around massive galaxies at early epochs and propose that the outer halo gas (>0.5 R

v
) was produced primarily in ancient satellite dwarf galaxy outflows, while the inner halo gas (<0.5 R

v
) originated from the central galaxy and persists as recycled accreting gas.
Observing Intermediate-mass Black Holes and the Upper Stellar-mass gap with LIGO and Virgo
Authors: Mehta Ajit Kumar , Buonanno Alessandra , Gair Jonathan , Miller M. Coleman , Farag Ebraheem , deBoer R. J. , Wiescher M. , Timmes F. X.
Published: January 2022

Using ground-based gravitational-wave detectors, we probe the mass function of intermediate-mass black holes (IMBHs) wherein we also include BHs in the upper mass gap at ∼60–130 M
⊙. Employing the projected sensitivity of the upcoming LIGO and Virgo fourth observing run (O4), we perform Bayesian analysis on quasi-circular nonprecessing, spinning IMBH binaries (IMBHBs) with total masses 50–500 M
⊙, mass ratios 1.25, 4, and 10, and dimensionless spins up to 0.95, and estimate the precision with which the source-frame parameters can be measured. We find that, at 2σ, the mass of the heavier component of IMBHBs can be constrained with an uncertainty of ∼10%–40% at a signal-to-noise ratio of 20. Focusing on the stellar-mass gap with new tabulations of the 12C(α, γ)16O reaction rate and its uncertainties, we evolve massive helium core stars using MESA to establish the lower and upper edges of the mass gap as ≃

59

−
13

+
34

M
⊙ and ≃

139

−
14

+
30

M
⊙ respectively, where the error bars give the mass range that follows from the ±3σ uncertainty in the 12C(α, γ)16O nuclear reaction rate. We find that high resolution of the tabulated reaction rate and fine temporal resolution are necessary to resolve the peak of the BH mass spectrum. We then study IMBHBs with components lying in the mass gap and show that the O4 run will be able to robustly identify most such systems. Finally, we reanalyze GW190521 with a state-of-the-art aligned-spin waveform model, finding that the primary mass lies in the mass gap with 90% credibility.
Core-collapse Supernova Simulations and the Formation of Neutron Stars, Hybrid Stars, and Black Holes
Authors: Kuroda Takami , Fischer Tobias , Takiwaki Tomoya , Kotake Kei
Published: January 2022

We investigate observable signatures of a first-order quantum chromodynamics (QCD) phase transition in the context of core-collapse supernovae. To this end, we conduct axially symmetric numerical relativity simulations with multi-energy neutrino transport, using a hadron–quark hybrid equation of state (EOS). We consider four nonrotating progenitor models, whose masses range from 9.6 to 70 M
⊙. We find that the two less-massive progenitor stars (9.6 and 11.2 M
⊙) show a successful explosion, which is driven by the neutrino heating. They do not undergo the QCD phase transition and leave behind a neutron star. As for the more massive progenitor stars (50 and 70 M
⊙), the proto-neutron star (PNS) core enters the phase transition region and experiences the second collapse. Because of a sudden stiffening of the EOS entering to the pure quark matter regime, a strong shock wave is formed and blows off the PNS envelope in the 50 M
⊙ model. Consequently the remnant becomes a quark core surrounded by hadronic matter, leading to the formation of the hybrid star. However, for the 70 M
⊙ model, the shock wave cannot overcome the continuous mass accretion and it readily becomes a black hole. We find that the neutrino and gravitational wave (GW) signals from supernova explosions driven by the hadron–quark phase transition are detectable for the present generation of neutrino and GW detectors. Furthermore, the analysis of the GW detector response reveals unique kHz signatures, which will allow us to distinguish this class of supernova explosions from failed and neutrino-driven explosions.
Cometary Activity beyond the Planets
Authors: Bouziani Naceur , Jewitt David
Published: January 2022

Recent observations show activity in long-period comet C/2017 K2 at heliocentric distances beyond the orbit of Uranus. With this as motivation, we constructed a simple model that takes a detailed account of gas transport modes and simulates the time-dependent sublimation of supervolatile ice from beneath a porous mantle on an incoming cometary nucleus. The model reveals a localized increase in carbon monoxide (CO) sublimation close to heliocentric distance r

H
= 150 au (local blackbody temperature ∼23 K), followed by a plateau and then a slow increase in activity toward smaller distances. This localized increase occurs as heat transport in the nucleus transitions between two regimes characterized by the rising temperature of the CO front at larger distances and nearly isothermal CO at smaller distances. As this transition is a general property of sublimation through a porous mantle, we predict that future observations of sufficient sensitivity will show that inbound comets (and interstellar interlopers) will exhibit activity at distances far beyond the planetary region of the solar system.
A Stellar Constraint on Eddington-inspired Born–Infeld Gravity from Cataclysmic Variable Binaries
Authors: Banerjee Pritam , Garain Debojyoti , Paul Suvankar , Shaikh Rajibul , Sarkar Tapobrata
Published: January 2022

Eddington-inspired Born–Infeld gravity is an important modification of Einstein’s general relativity, which can give rise to nonsingular cosmologies at the classical level, and avoid the end-stage singularity in a gravitational collapse process. In the Newtonian limit, this theory gives rise to a modified Poisson’s equation, as a consequence of which stellar observables acquire model dependent corrections, compared to the ones computed in the low energy limit of general relativity. This can in turn be used to establish astrophysical constraints on the theory. Here, we obtain such a constraint using observational data from cataclysmic variable binaries. In particular, we consider the tidal disruption limit of the secondary star by a white dwarf primary. The Roche lobe filling condition of this secondary star is used to compute stellar observables in the modified gravity theory in a numerical scheme. These are then contrasted with the values obtained by using available data on these objects, via a Monte Carlo error progression method. This way, we are able to constrain the theory within the 5σ confidence level.
Investigation of the Timing and Spectral Properties of an Ultraluminous X-Ray Pulsar NGC 7793 P13
Authors: Lin Lupin Chun-Che , Hu Chin-Ping , Takata Jumpei , Li Kwan-Lok , Hui C. Y. , Kong A. K. H.
Published: January 2022

We perform both timing and spectral analyses using the archival X-ray data taken with Swift, XMM-Newton, NICER, and NuSTAR from 2016 to 2020 to study an ultraluminous pulsar, NGC 7793 P13, that showed a long period of super-Eddington accretion. We use the Rayleigh test to investigate the pulsation at different epochs, and confirm the variation of the pulse profile with finite Gaussian mixture modeling and a two-sample Kuiper test. Taking into account the periodic variation of the spin periods caused by the orbital Doppler effect, we further determine an orbital period of ∼65 days and show that no significant correlation can be detected between the orbital phase and the pulsed fraction. The pulsed spectrum of NGC 7793 P13 in the 0.5–20 keV range can be simply described using a power law with a high-energy exponential cutoff, while the broadband phase-averaged spectrum of the same energy range requires two additional components to account for the contribution of a thermal accretion disk and the Comptonization photons scattered into the hard X-rays. We find that NGC 7793 P13 stayed in the hard ultraluminous state and the pulsed spectrum was relatively soft when the source was faint at the end of 2019. Moreover, an absorption feature close to 1.3 keV is marginally detected from the pulsed spectra and it is possibly associated with a cyclotron resonant scattering feature.
Sculpting the Sub-Saturn Occurrence Rate via Atmospheric Mass Loss
Authors: Hallatt Tim , Lee Eve J.
Published: January 2022

The sub-Saturn (∼4–8 R
⊕) occurrence rate rises with orbital period out to at least ∼300 days. In this work we adopt and test the hypothesis that the decrease in their occurrence toward the star is a result of atmospheric mass loss, which can transform sub-Saturns into sub-Neptunes (≲4 R
⊕) more efficiently at shorter periods. We show that under the mass-loss hypothesis, the sub-Saturn occurrence rate can be leveraged to infer their underlying core mass function, and, by extension, that of gas giants. We determine that lognormal core mass functions peaked near ∼10–20 M
⊕ are compatible with the sub-Saturn period distribution, the distribution of observationally inferred sub-Saturn cores, and gas-accretion theories. Our theory predicts that close-in sub-Saturns should be ∼50% less common and ∼30% more massive around rapidly rotating stars; this should be directly testable for stars younger than ≲500 Myr. We also predict that the sub-Jovian desert becomes less pronounced and opens up at smaller orbital periods around M stars compared to solar-type stars (∼0.7 days versus ∼3 days). We demonstrate that exceptionally low-density sub-Saturns, “super-puffs,” can survive intense hydrodynamic escape to the present day if they are born with even larger atmospheres than they currently harbor; in this picture, Kepler 223 d began with an envelope ∼1.5× the mass of its core and is currently losing its envelope at a rate of ∼2 × 10−3
M
⊕ Myr−1. If the predictions from our theory are confirmed by observations, the core mass function we predict can also serve to constrain core formation theories of gas-rich planets.
GASP XXXVIII: The LOFAR-MeerKAT-VLA View on the Nonthermal Side of a Jellyfish Galaxy
Authors: Ignesti Alessandro , Vulcani Benedetta , Poggianti Bianca M. , Paladino Rosita , Shimwell Timothy , Healy Julia , Gitti Myriam , Bacchini Cecilia , Moretti Alessia , Radovich Mario , van Weeren Reinout J. , Roberts Ian D. , Botteon Andrea , Müller Ancla , McGee Sean , Fritz Jacopo , Tomičić Neven , Werle Ariel , Mingozzi Matilde , Gullieuszik Marco , Verheijen Marc
Published: January 2022

Ram pressure stripping is a crucial evolutionary driver for cluster galaxies. It is thought to be able to accelerate the evolution of their star formation, trigger the activity of their central active galactic nucleus (AGN) and the interplay between galactic and environmental gas, and eventually dissipate their gas reservoirs. We explored the outcomes of ram pressure stripping by studying the nonthermal radio emission of the jellyfish galaxy JW100 in the cluster A2626 (z = 0.055), by combining LOw Frequency Array, MeerKAT, and Very Large Array observations from 0.144 to 5.5 GHz. We studied the integrated spectra of the stellar disk, the stripped tail, and the AGN; mapped the spectral index over the galaxy; and constrained the magnetic field intensity to between 11 and 18 μG in the disk and <10 μG in the tail. The stellar disk radio emission is dominated by a radiatively old plasma, likely related to an older phase of a high star formation rate. This suggests that the star formation was quickly quenched by a factor of 4 in a few 107 yr. The radio emission in the tail is consistent with the stripping scenario, where the radio plasma that originally accelerated in the disk is subsequently displaced in the tail. The morphology of the radio and X-ray emissions supports the scenario of the accretion of magnetized environmental plasma onto the galaxy. The AGN nonthermal spectrum indicates that relativistic electron acceleration may have occurred simultaneously with a central ionized gas outflow, thus suggesting a physical connection between the two processes.
Meridional Circulation of Dust and Gas in the Circumstellar Disk: Delivery of Solids onto the Circumplanetary Region
Authors: Szulágyi J. , Binkert F. , Surville C.
Published: January 2022

We carried out 3D dust + gas radiative hydrodynamic simulations of forming planets. We investigated a parameter grid of a Neptune-mass, a Saturn-mass, a Jupiter-mass, and a five-Jupiter-mass planet at 5.2, 30, and 50 au distance from their star. We found that the meridional circulation (Szulágyi et al. 2014; Fung & Chiang 2016) drives a strong vertical flow for the dust as well, hence the dust is not settled in the midplane, even for millimeter-sized grains. The meridional circulation will deliver dust and gas vertically onto the circumplanetary region, efficiently bridging over the gap. The Hill-sphere accretion rates for the dust are ∼10−8–10−10
M
Jup yr−1, increasing with planet mass. For the gas component, the gain is 10−6–10−8
M
Jup yr−1. The difference between the dust and gas-accretion rates is smaller with decreasing planetary mass. In the vicinity of the planet, the millimeter-sized grains can get trapped easier than the gas, which means the circumplanetary disk might be enriched with solids in comparison to the circumstellar disk. We calculated the local dust-to-gas ratio (DTG) everywhere in the circumstellar disk and identified the altitude above the midplane where the DTG is 1, 0.1, 0.01, and 0.001. The larger the planetary mass, the more the millimeter-sized dust is delivered and a larger fraction of the dust disk is lifted by the planet. The stirring of millimeter-sized dust is negligible for Neptune-mass planets or below, but significant above Saturn-mass planets.
Evolution of Plasma Composition in an Eruptive Flux Rope
Authors: Baker D. , Green L. M. , Brooks D. H. , Démoulin P. , van Driel-Gesztelyi L. , Mihailescu T. , To A. S. H. , Long D. M. , Yardley S. L. , Janvier M. , Valori G.
Published: January 2022

Magnetic flux ropes are bundles of twisted magnetic field enveloping a central axis. They harbor free magnetic energy and can be progenitors of coronal mass ejections (CMEs). However, identifying flux ropes on the Sun can be challenging. One of the key coronal observables that has been shown to indicate the presence of a flux rope is a peculiar bright coronal structure called a sigmoid. In this work, we show Hinode EUV Imaging Spectrometer observations of sigmoidal active region (AR) 10977. We analyze the coronal plasma composition in the AR and its evolution as a sigmoid (flux rope) forms and erupts as a CME. Plasma with photospheric composition was observed in coronal loops close to the main polarity inversion line during episodes of significant flux cancellation, suggestive of the injection of photospheric plasma into these loops driven by photospheric flux cancellation. Concurrently, the increasingly sheared core field contained plasma with coronal composition. As flux cancellation decreased and a sigmoid/flux rope formed, the plasma evolved to an intermediate composition in between photospheric and typical AR coronal compositions. Finally, the flux rope contained predominantly photospheric plasma during and after a failed eruption preceding the CME. Hence, plasma composition observations of AR 10977 strongly support models of flux rope formation by photospheric flux cancellation forcing magnetic reconnection first at the photospheric level then at the coronal level.