Miracle-dz/UniFAR-FTUs huggingface dataset:
HOW EMPTY ARE DISK GAPS OPENED BY GIANT PLANETS

Gap clearing by giant planets has been proposed to explain the optically thin cavities observed in many protoplanetary disks. How much material remains in the gap determines not only how detectable young planets are in their birth environments, but also how strong co-rotation torques are, which impacts how planets can survive fast orbital migration. We determine numerically how the average surface density inside the gap, Σ{sub gap}, depends on planet-to-star mass ratio q, Shakura-Sunyaev viscosity parameter α, and disk height-to-radius aspect ratio h/r. Our results are derived from our new graphics processing unit accelerated Lagrangian hydrodynamical code PEnGUIn and are verified by independent simulations with ZEUS90. For Jupiter-like planets, we find Σ{sub gap}∝q {sup –2.2}α{sup 1.4}(h/r){sup 6.6}, and for near brown dwarf masses, Σ{sub gap}∝q {sup –1}α{sup 1.3}(h/r){sup 6.1}. Surface density contrasts inside and outside gaps can be as large as 10{sup 4}, even when the planet does not accrete. We derive a simple analytic scaling, Σ{sub gap}∝q {sup –2}α{sup 1}(h/r){sup 5}, that compares reasonably well to empirical results, especially at low Neptune-like masses, and use discrepancies to highlight areas for progress.
The transient neutron star X-ray binary KS 1741–293 in outburst and quiescence

Abstract KS 1741–293 is a transient neutron star low-mass X-ray binary that is located at an angular distance of ≃20′ from the Galactic center. We map out the historic activity of the source since its discovery in 1989, characterize its most recent X-ray outbursts observed with Swift (2007, 2008, 2010, and 2011), and discuss its quiescent X-ray properties using archival Chandra data. KS 1741–293 is frequently active, exhibiting outbursts that typically reach a 2–10 keV luminosity of LX ≃ 1036 (D/6.2 kpc)2 erg s−1 and last for several weeks–months. However, Swift also captured a very short and weak accretion outburst that had a duration of ≲4 days and did not reach above LX ≃ 5×1034 (D/6.2 kpc)2 erg s−1. The source is detected in quiescence with Chandra at a 2–10 keV luminosity of LX ≃ 2.5×1032 (D/6.2 kpc)2 erg s−1.
Interstellar matter and star formation in W5-E - A Herschel view

W5-E has been observed with the Herschel-PACS and -SPIRE photometers, at 100, 160, 250, 350, and 500 microns. The dust temperature map shows a rather uniform temperature, in the range 17.5-20 K in the dense condensations or filaments, 21-22 K in the photodissociation regions, and 24-31 K in the direction of the ionized regions. The column densities are rather low, everywhere lower than 10^23 cm-2, and of the order of a few 10^21 cm-2 in the PDRs. About 8000 solar masses of neutral material surrounds the ionized region, which is low with respect to the volume of this HII region; we suggest that the exciting stars of the W5-E, W5-W, Sh~201, A and B HII regions formed along a dense filament or sheet rather than inside a more spherical cloud. Fifty point sources have been detected at 100 microns. Most of them are Class 0/I YSOs. The SEDs of their envelopes have been fitted using a modified blackbody model. These envelopes are cold, with a mean temperature of 15.7+-1.8K. Their masses are in the range 1.3-47 solar masses. Eleven of these point sources are candidate Class 0 YSOs. Twelve of these point sources are possibly at the origin of bipolar outflows detected in this region. None of the YSOs contain a massive central object, but a few may form a massive star as they have both a massive envelope and also a high envelope accretion rate. Most of the Class 0/I YSOs are observed in the direction of high column density material, for example in the direction of the massive condensations present at the waist of the bipolar Sh 201 HII region or enclosed by the bright-rimmed cloud BRC14. The overdensity of Class 0/I YSOs on the borders of the HII regions strongly suggests that triggered star formation is at work in this region but, due to insufficient resolution, the exact processes at the origin of the triggering are difficult to determine.
Relationship between burnout, effort-reward imbalance, and insomnia among Informational Technology professionals

BACKGROUND: Work in informational technology (IT) professionals is highly competitive and stressful, leading to job stress. This can lead to burnout, effort-reward imbalance (ERI), and poor sleep quality. MATERIALS AND METHODS: The present study examined associations of ERI, burnout, and poor sleep quality among IT professionals using data from 200 software engineers (mean age of 29.3 ± 4 years, 32% women). ERI and overcommitment were assessed using Siegrist's “effort-reward” questionnaire. The Oldenburg Burnout Inventory (OLBI) was used to assess burnout and Pittsburgh Sleep Quality Index (PSQI) to assess sleep quality. RESULTS: ERI, burnout and poor sleep quality were present in 72%, 60%, and 70%, respectively. Females had higher ERI, burnout, and poor sleep quality compared to males. ERI is significantly associated with burnout (r = 0.45, P < 0.01) and poor sleep quality (r = 0.31, P < 0.01). Linear regression to assess the ability of ERI to predict levels of burnout yielded a statistically significant (R2 = 0.206, P < 0.01) indicating ERI to be a unique incremental predictor of burnout (b = 0.454, t = 7.16, P < 0.01). ERI tends to be a predictive factor of poor sleep quality with Odd's ratio = 3.5, 95%CI (1.81–6.73), P < 0.01. CONCLUSION: In summary, Intervention programs both at the individual and at the organization level have to be designed to combat ERI, burnout, and poor sleep quality among IT professionals.
A unified secondary electron cut-off presentation and common mistakes in photoelectron spectroscopy

Photoelectron spectroscopy is a powerful surface analysis technique that can differentiate different bonding environments and directly determine the absolute work function of a sample. Despite its ever-easier accessibility—or perhaps precisely because of it—some common mistakes or bad habits are often found in the literature when it comes to the evaluation or presentation of photoelectron spectroscopy data. Here we address some of these issues and give suggestions for best practice, i.e., a proper presentation of the secondary electron cut-off used for work function determination, correct binding energy referencing and some tips for appropriate peak fitting, as well as valuable literature references to more detailed tutorials. Finally, we present a concise step-by-step guide on how to conduct a complete x-ray photoelectron spectroscopy analysis of an unknown sample.
Methods and Practices for In Situ Measurements of RF EMF Exposure From 5G Millimeter Wave Base Stations

In this article, a methodology for in situ measurements of the radio frequency electromagnetic fields exposure from 5G base stations (BSs) operating at millimeter wave (mmW) frequencies is presented. Measurements were performed in proximity of two BSs operating around 28 and 39 GHz. The measured power density from the BSs when extrapolated for the maximum transmit power was below 30 mW/m2 at a distance of about 10 m (i.e., below 1% of the ICNIRP limits). A systematic analysis of the challenges related to in situ measurements of 5G mmW exposure is conducted for the first time. It was found that exposure measurement procedures developed for frequencies below 6 GHz (such as those based on extrapolation of the synchronization signal block) are generally applicable also at mmW. When in line-of-sight, dual-polarized directional antennas can be used to accurately characterize the maximum exposure. The angular variation of the incident power density at the measurement location was studied by means of a motor-controlled panorama tilt unit. At the same time, a network counter was used to monitor the directional time-averaged power transmitted by the BS. The study is of importance to standardization committees addressing measurement techniques to assess exposure from mobile networks.
Cross sex hormone treatment is linked with a reversal of cerebral patterns associated with gender dysphoria to the baseline of cisgender controls

Transgender persons experience incongruence between their gender identity and birth‐assigned sex. The resulting gender dysphoria (GD), is frequently treated with cross‐sex hormones. However, very little is known about how this treatment affects the brain of individuals with GD, nor do we know the neurobiology of GD. We recently suggested that disconnection of fronto‐parietal networks involved in own‐body self‐referential processing could be a plausible mechanism, and that the anatomical correlate could be a thickening of the mesial prefrontal and precuneus cortex, which is unrelated to sex. Here, we investigate how cross‐sex hormone treatment affects cerebral tissue in persons with GD, and how potential changes are related to self‐body perception. Longitudinal MRI measurements of cortical thickness (Cth) were carried out in 40 transgender men (TrM), 24 transgender women (TrW) and 19 controls. Cth increased in the mesial temporal and insular cortices with testosterone treatment in TrM, whereas anti‐androgen and oestrogen treatment in TrW caused widespread cortical thinning. However, after correction for treatment‐related changes in total grey and white matter volumes (increase with testosterone; decrease with anti‐androgen and oestrogen), significant Cth decreases were observed in the mesial prefrontal and parietal cortices, in both TrM and TrW (vs. controls) – regions showing greater pre‐treatment Cth than in controls. The own body – self congruence ratings increased with treatment, and correlated with a left parietal cortical thinning. These data confirm our hypothesis that GD may be associated with specific anatomical features in own‐body/self‐processing circuits that reverse to the pattern of cisgender controls after cross‐sex hormone treatment.
Natural convection with mixed insulating and conducting boundary conditions: low- and high-Rayleigh-number regimes

Abstract We investigate the stability and dynamics of natural convection in two dimensions, subject to inhomogeneous boundary conditions. In particular, we consider a Rayleigh–Bénard (RB) cell, where the horizontal top boundary contains a periodic sequence of alternating thermal insulating and conducting patches, and we study the effects of the heterogeneous pattern on the global heat exchange, at both low and high Rayleigh numbers. At low Rayleigh numbers, we determine numerically the transition from a regime characterized by the presence of small convective cells localized at the inhomogeneous boundary to the onset of ‘bulk’ convective rolls spanning the entire domain. Such a transition is also controlled analytically in the limit when the boundary pattern length is small compared with the cell vertical size. At higher Rayleigh number, we use numerical simulations based on a lattice Boltzmann method to assess the impact of boundary inhomogeneities on the fully turbulent regime up to $\mathit{Ra} \sim 10^{10}$ .
Microvascular morphology alteration using relaxation rate change with gadolinium-based magnetic resonance imaging contrast agent in patients with Alzheimer’s disease

Background Conventional magnetic resonance imaging (MRI) techniques cannot demonstrate microvascular alterations in mild Alzheimer’s disease (AD). Thus, the diagnosis of microvascular pathology commonly relies on postmortem. The purpose of this study was to evaluate alterations of microvascular structures in patients with AD using a 3T clinical MRI system with a commercially available contrast agent. Methods Eleven patients with AD and 11 cognitively normal (CN) controls were included in this cross-sectional prospective study. R2 and R2* relaxation rate changes (∆R2 and ∆R2*) before and after a Gadolinium (Gd)-based contrast agent injection were calculated from images obtained with a multi-echo turbo spin-echo sequence and multi-echo gradient-echo sequence to obtain microvascular index maps of blood volume fraction (BVf), mean vessel diameter (mVD), vessel size index (VSI), mean vessel density (Q), and microvessel-weighted imaging (MvWI). Two-sample t-test was used to compare those values between the two groups. Correlation analysis was performed to evaluate the relationship between those values and age. Results BVfs at the corpus callosum and at the thalamus were significantly increased in the AD group (P=0.024 and P=0.005, respectively). BVf at the gray matter (P=0.020) and white matter area (P=0.012) were also significantly increased in the AD group compared with the CN group. MvWIs at the hippocampus and parahippocampal gyrus were significantly increased in the AD group compared with the CN group (P=0.020 and P=0.006, respectively). Voxel-based analysis showed both mVD and VSI were significantly decreased at the prefrontal lobe in the AD group. Q were not significant difference between CN and AD groups. MvWI were significantly positively correlated with age. Conclusions Microvascular index was a useful non-invasive method to evaluate microvascular morphology alteration. The microvascular morphology of AD was manifested as increasing BVf and microvessel-weighted.
Nitrogen line spectroscopy of O-stars - II. Surface nitrogen abundances for O-stars in the Large Magellanic Cloud

This is the second paper in a series aiming at the analysis of nitrogen abundances in O-type stars, to enable further constraints on the early evolution of massive stars. We investigate the NIV lambda4058 emission line formation, provide nitrogen abundances for a substantial O-star sample in the LMC, and compare our findings with recent predictions from stellar evolutionary models. Stellar and wind parameters are determined by line profile fitting of hydrogen, helium and nitrogen lines, based on synthetic spectra calculated by FASTWIND. We derive nitrogen abundances for 20 O- and 5 B-stars, by analyzing all nitrogen lines present in the available optical spectra. The dominating process responsible for emission at NIV lambda4058 in O-stars is the strong depopulation of the lower level of the transition, which increases as a function of Mdot. Unlike the NIII triplet emission, resonance lines do not play a role for typical mass-loss rates and below. The bulk of our sample O-stars seems to be strongly nitrogen-enriched, and a clear correlation of nitrogen and helium enrichment is found. By comparing the nitrogen abundances as a function of vsini ('Hunter-plot') with tailored evolutionary calculations, we identify a considerable number of highly enriched objects at low rotation. Due to the low initial abundance, the detection of strong Nitrogen enrichment in the bulk of O-stars indicates that efficient mixing takes place already during the very early phases of stellar evolution of LMC O-stars.
Meta Analisis Model Problem Based Learning Dalam Meningkatkan Kemampuan Berpikir Kritis Pada Pembelajaran Matematika

Model Problem Based Learning telah banyak digunakan sebagai solusi dalam meningkatkan kemampuan berpikir kritis. Namun, belum ada penelitian lanjutan yang melakukan verifikasi terhadap efektivitas hasil penerapan model Problem Based Learning. Penelitian ini bertujuan untuk menganalisis kembali keefektifan model pembelajaran Problem Based Learning terhadap kemampuan berpikir kritis siswa pada pelajaran Matematika khususnya pada siswa sekolah dasar. Metode yang digunakan dalam penelitian ini adalah meta-analisis secara analisis deskriptif kualitatif, yaitu dengan menganalisis kembali artikel dari hasil penelitian yang telah dipublikasikan dengan sampel sebanyak 20 artikel nasional dan dapat diakses secara online melalui Google Scholar atau Google Cendekia. Hasil dari penelitian meta-analisis ini menunjukkan bahwa model pembelajaran Problem Based Learning sangat berpengaruh dalam meningkatkan kemampuan berpikir kritis siswa pada pelajaran matematika sekolah dasar dengan presentase terendah 1,16% hingga yang tertinggi 40,35% dengan rata rata 20,70%. Berdasarkan hasil analisis, secara keseluruhan rata-rata pengaruh yang terdapat pada model pembelajaran Problem Based Learning sebesar 1,21. Sehingga dapat disimpulkan bahwa model Problem Based Learning efektif dalam meningkatkan kemampuan berpikir kritis siswa pada mata pelajaran matematika.
Cecinothofagus Nieves-Aldrey & Liljeblad (Hymenoptera, Cynipidae) is likely an endoparasitoid of the gall-maker genus Aditrochus Rübsaamen (Hymenoptera, Pteromalidae)

Paraulax Kieffer and Cecinothofagus Nieves-Aldrey & Liljeblad (Cynipidae: Paraulacini) were long supposed to be gall-makers on southern beeches ( Nothofagus , Nothofagaceae). Dissections of galls on Nothofagus Blume, suggested that Cecinothofagus could be instead either endoparasitoid or inquiline of Aditrochus larva (Chalcidoidea). We sequenced the universal COI barcode and Ultra-Conserved Elements (UCEs) from young larvae of Aditrochus collected from galls on Nothofagus and highlighted that one of them also contained DNA from Cecinothofagus ibarrai Nieves-Aldrey & Liljeblad. So far, when galls attributed to Aditrochus were dissected in early development stages they all contained only a single larva and no remains of other larvae. Conversely, when Cecinothofagus ibarrai was reared from galls on Nothofagus , remains of the host larva were observed inside the larval chamber. Altogether, biological observations and molecular results suggest that Cecinothofagus ibarrai is likely an endoparasitoid of Adritrochus . This result confirms the tribe Paraulacini as being entomophagous and supports the hypothesis of an ancestral parasitoid lifestyle for Cynipoidea.
Sobolev solutions of parabolic equation in a complete riemannian manifold

We study Sobolev estimates for the solutions of parabolic equations acting on a vector bundle, in a complete riemannian manifold $M. $ The idea is to use known estimates in ${\mathbb{R}}^{n}$ to get local estimates on $M$ and then to use our LIR method to get the global estimates we are searching for. As an application, we give Sobolev estimates for the solutions of the heat equation on $p$-forms in complete non-compact riemannian manifold.
Rabi oscillation induced $π$-phase flip in an unbalanced Ramsey atom interferometer

We present an observation of zero-to-$\ensuremath{\pi}$ phase flips induced by Rabi oscillation in an unbalanced Ramsey atom interferometer. The phase shift and visibility are experimentally investigated by modulating either the polarization or duration of Raman lasers, and they are well explained by a theoretical model. In an atom interferometer, the $\ensuremath{\pi}$ phase flips are caused not only by the sign of Rabi frequency but also by the Rabi oscillation. Considering the $\ensuremath{\pi}$ phase flips, we propose the composite-light-pulse sequences for realizing the large-momentum-transfer beam splitter and mirror, which have the high immunity to the external phase noise in building the cold atom interferometer.
INTEGRATED OPTICAL POLARIZATION OF NEARBY GALAXIES

We performed an integrated optical polarization survey of 70 nearby galaxies to study the relationship between linear polarization and galaxy properties. To date this is the largest survey of its kind. The data were collected at McDonald Observatory using the Imaging Grism Polarimeter on the Otto Struve 2.1 m telescope. Most of the galaxies did not have significant level of linear polarization, where the bulk is <1%. A fraction of the galaxies showed a loose correlation between the polarization and position angle of the galaxy, indicating that dust scattering is the main source of optical polarization. The unbarred spiral galaxies are consistent with the predicted relationship with inclination from scattering models of ∼sin 2i.
RADIAL VELOCITIES OF THREE POORLY STUDIED CLUSTERS AND THE KINEMATICS OF OPEN CLUSTERS

We present radial velocities for stars in the field of the open star clusters Berkeley 44, Berkeley 81, and NGC 6802 from spectra obtained using the Wisconsin–Indiana–Yale–NOAO (WIYN) 3.5 m telescope. These clusters are of intermediate age (1–3 Gyr), located within the solar Galactocentric radius, and have no previous radial velocity measurements. We find mean radial velocities of −9.6 ± 3.0 km s−1, 48.1 ± 2.0 km s−1, and 12.4 ± 2.8 km s−1 for Be 44, Be 81, and NGC 6802, respectively. We present an analysis of radial velocities of 134 open clusters of a wide range of ages using data obtained in this study and the literature. Assuming the system of clusters rotates about the Galactic center with a constant velocity, we find older clusters exhibit a slower rotation and larger line-of-sight (LOS) velocity dispersion than younger clusters. The gradual decrease in rotational velocity of the cluster system with age is accompanied by a smooth increase in LOS velocity dispersion, which we interpret as the effect of heating on the open cluster system over time.
A Strengthened PAKE Protocol with Identity-Based Encryption

SUMMARY In [2], Choi et al. proposed an identity-based password-authenticated key exchange (iPAKE) protocol using the Boneh-Franklin IBE scheme, and its generic construction (UKAM-PiE) that was standardized in ISO / IEC 11770-4 / AMD 1. In this paper, we show that the iPAKE and UKAM-PiE protocols are insecure against passive / active attacks by a malicious PKG (Private Key Generator) where the malicious PKG can ﬁnd out all clients’ passwords by just eavesdropping on the communications, and the PKG can share a session key with any client by impersonating the server. Then, we propose a strengthened PAKE (for short, SPAIBE ) protocol with IBE, which prevents such a malicious PKG’s passive / active attacks. Also, we formally prove the security of the SPAIBE protocol in the random oracle model and compare relevant PAKE protocols in terms of e ﬃ ciency, number of passes, and security against a malicious PKG.
CHANGE OF MAGNETIC FIELD-GAS ALIGNMENT AT THE GRAVITY-DRIVEN ALFVÉNIC TRANSITION IN MOLECULAR CLOUDS: IMPLICATIONS FOR DUST POLARIZATION OBSERVATIONS

Diffuse striations in molecular clouds are preferentially aligned with local magnetic fields, whereas dense filaments tend to be perpendicular to them. When and why this transition occurs remain uncertain. To explore the physics behind this transition, we compute the histogram of relative orientation (HRO) between the density gradient and the magnetic field in three-dimensional magnetohydrodynamic (MHD) simulations of prestellar core formation in shock-compressed regions within giant molecular clouds. We find that, in the magnetically dominated (sub-Alfvénic) post-shock region, the gas structure is preferentially aligned with the local magnetic field. For overdense sub-regions with super-Alfvénic gas, their elongation becomes preferentially perpendicular to the local magnetic field. The transition occurs when self-gravitating gas gains enough kinetic energy from the gravitational acceleration to overcome the magnetic support against the cross-field contraction, which results in a power-law increase of the field strength with density. Similar results can be drawn from HROs in projected two-dimensional maps with integrated column densities and synthetic polarized dust emission. We quantitatively analyze our simulated polarization properties, and interpret the reduced polarization fraction at high column densities as the result of increased distortion of magnetic field directions in trans- or super-Alfvénic gas. Furthermore, we introduce measures of the inclination and tangledness of the magnetic field along the line of sight as the controlling factors of the polarization fraction. Observations of the polarization fraction and angle dispersion can therefore be utilized in studying local magnetic field morphology in star-forming regions.
Medium mass fragments production due to momentum dependent interactions

The role of system size and momentum dependent effects are analyzed in multifragmenation by simulating symmetric reactions of Ca+Ca, Ni+Ni, Nb+Nb, Xe+Xe, Er+Er, Au+Au, and U+U at incident energies between 50 MeV/nucleon and 1000 MeV/nucleon and over full impact parameter zones. Our detailed study reveals that there exist a system size dependence when reaction is simulated with momentum dependent interactions. This dependence exhibits a mass power law behavior.