Miracle-dz/UniFAR-FTUs huggingface dataset:
ECCENTRIC JUPITERS VIA DISK–PLANET INTERACTIONS

Numerical hydrodynamics calculations are performed to determine the conditions under which giant planet eccentricities can be excited by parent gas disks. Unlike in other studies, Jupiter-mass planets are found to have their eccentricities amplified—provided their orbits start off as eccentric. We disentangle the web of co-rotation, co-orbital, and external resonances to show that this finite-amplitude instability is consistent with that predicted analytically. Ellipticities can grow until they reach of order of the disk's aspect ratio, beyond which the external Lindblad resonances that excite eccentricity are weakened by the planet's increasingly supersonic epicyclic motion. Forcing the planet to still larger eccentricities causes catastrophic eccentricity damping as the planet collides into gap walls. For standard parameters, the range of eccentricities for instability is modest; the threshold eccentricity for growth (∼0.04) is not much smaller than the final eccentricity to which orbits grow (∼0.07). If this threshold eccentricity can be lowered (perhaps by non-barotropic effects), and if the eccentricity driving documented here survives in 3D, it may robustly explain the low-to-moderate eccentricities ≲0.1 exhibited by many giant planets (including Jupiter and Saturn), especially those without planetary or stellar companions.
Baryon Axial Charges and Momentum Fractions with N_f=2+1 Dynamical Fermions

We report on recent results of the QCDSF/UKQCD Collaboration on investigations of baryon structure using configurations generated with N_f=2+1 dynamical flavours of O(a) improved Wilson fermions. With the strange quark mass as an additional dynamical degree of freedom in our simulations we avoid the need for a partially quenched approximation when investigating the properties of particles containing a strange quark, e.g. the hyperons. In particular, we will focus on the nucleon and hyperon axial charges and quark momentum fractions.
EVOLUTION OF THERMALLY PULSING ASYMPTOTIC GIANT BRANCH STARS. IV. CONSTRAINING MASS LOSS AND LIFETIMES OF LOW MASS, LOW METALLICITY AGB STARS

The evolution and lifetimes of thermally pulsating asymptotic giant branch (TP-AGB) stars suffer from significant uncertainties. In this work, we analyze the numbers and luminosity functions of TP-AGB stars in six quiescent, low metallicity ([Fe/H] ≲ −0.86) galaxies taken from the ACS Nearby Galaxy Survey Treasury sample, using Hubble Space Telescope (HST) photometry in both optical and near-infrared filters. The galaxies contain over 1000 TP-AGB stars (at least 60 per field). We compare the observed TP-AGB luminosity functions and relative numbers of TP-AGB and red giant branch (RGB) stars, NTP-AGB/NRGB, to models generated from different suites of TP-AGB evolutionary tracks after adopting star formation histories derived from the HST deep optical observations. We test various mass-loss prescriptions that differ in their treatments of mass loss before the onset of dust-driven winds (pre-dust). These comparisons confirm that pre-dust mass loss is important, since models that neglect pre-dust mass loss fail to explain the observed NTP-AGB/NRGB ratio or the luminosity functions. In contrast, models with more efficient pre-dust mass loss produce results consistent with observations. We find that for [Fe/H] ≲ −0.86, lower mass TP-AGB stars (M ≲ 1 M☉) must have lifetimes of ∼0.5 Myr and higher masses (M ≲ 3 M☉) must have lifetimes ≲ 1.2 Myr. In addition, assuming our best-fitting mass-loss prescription, we show that the third dredge-up has no significant effect on TP-AGB lifetimes in this mass and metallicity range.
Nonlinear evolution equations: Global behavior of solutions

Generalities and local theory. - The global existence problem. - Theory of monotone operators and applications. - Smoothing effect for some nonlinear evolution equations. - Schrodinger and wave equations with a logarithmic nonlinearity. - The linear case: Hilbertian theory and applications. - Some nonlinear monotone cases. - Some nonlinear, non monotone cases. - Autonomous dissipative systems. - General results for quasi-autonomous periodic systems. - More on asymptotic behavior for solutions of the nonlinear dissipative forced wave equation. - Boundedness of trajectories for quasi-autonomous dissipative systems. - Almost-periodic quasi-autonomous dissipative systems in a Hilbert space.
Critical branching processes evolving in an unfavorable random environment

Let { Z n , n = 0 , 1 , 2 , . } be a critical branching process in random environment and let { S n , n = 0 , 1 , 2 , . } be its associated random walk. It is known that if the increments of this random walk belong (without cen-tering) to the domain of attraction of a stable law, then there exists a sequence a 1 , a 2 , . , slowly varying at inﬁnity such that the conditional distributions ) weakly converges, as n → ∞ to the distribution of a strictly positive and proper random variable. In this paper we supplement this result with a description of the asymptotic behavior of the probability P ( S n ≤ ϕ ( n ); Z n > 0) , if ϕ ( n ) → ∞ as n → ∞ in such a way that ϕ ( n ) = o ( a n ).
Revisiting the Logarithmic Corrections to the Black Hole Entropy

Logarithmic corrections to the entropy of extremal black holes have been successfully used to accurately match degeneracies from microscopic constructions to calculations of the gravitational path integral. In this paper, we revisit the problem of deriving such corrections for the case of extremal black holes, either non-supersymmetric or supersymmetric, and for near-extremal black holes. The zero-modes that are present at extremality are crucial, since their path integral cannot be treated quadratically and needs to be regulated. We show how the regulated result can be obtained by taking the zero-temperature limit of either the 4 d Einstein-Maxwell or 4 d supergravity path integral to ﬁnd the Schwarzian or super-Schwarzian theories. This leads to drastically diﬀerent estimates for the degeneracy of non-supersymmetric and supersymmetric extremal black holes. In a companion paper, we discuss how such zero-modes aﬀect the calculation of BPS black holes degeneracies, using supersymmetric localization for an exact computation of the gravitational path integral.
No Peaks without Valleys: The Stable Mass Transfer Channel for Gravitational-wave Sources in Light of the Neutron Star–Black Hole Mass Gap

Gravitational-wave (GW) detections are starting to reveal features in the mass distribution of double compact objects. The lower end of the black hole (BH) mass distribution is especially interesting as few formation channels contribute here and because it is more robust against variations in the cosmic star formation than the high-mass end. In this work we explore the stable mass transfer channel for the formation of GW sources with a focus on the low-mass end of the mass distribution. We conduct an extensive exploration of the uncertain physical processes that impact this channel. We note that, for fiducial assumptions, this channel reproduces the peak at ∼9 M ☉ in the GW-observed binary BH mass distribution remarkably well and predicts a cutoff mass that coincides with the upper edge of the purported neutron star–black hole (NS–BH) mass gap. The peak and cutoff mass are a consequence of the unique properties of this channel; namely (1) the requirement of stability during the mass transfer phases, and (2) the complex way in which the final compact object masses scale with the initial mass. We provide an analytical expression for the cutoff in the primary component mass and show that this adequately matches our numerical results. Our results imply that selection effects resulting from the formation channel alone can provide an explanation for the purported NS–BH mass gap in GW detections. This provides an alternative to the commonly adopted view that the gap emerges during BH formation.
Measures of Galaxy Environment I - What is "Environment"?

The influence of a galaxy’s environment on its evolution has been studied and compared extensively in the literature, although differing techniques are often used to define environment. Most methods fall into two broad groups: those that use nearest neighbours to probe the underlying density field and those that use fixed apertures. The differences between the two inhibit a clean comparison between analyses and leave open the possibility that, even with the same data, different properties are actually being measured. In this work we apply twenty published environment definitions to a common mock galaxy catalogue constrained to look like the local Universe. We find that nearest neighbour-based measures best probe the internal densities of high-mass haloes, while at low masses the inter-halo separation dominates and acts to smooth out local density variations. The resulting correlation also shows that nearest neighbour galaxy environment is largely independent of dark matter halo mass. Conversely, aperture-based methods that probe super-halo scales accurately identify high-density regions corresponding to high mass haloes. Both methods show how galaxies in dense environments tend to be redder, with the exception of the largest apertures, but these are the strongest at recovering the background dark matter environment. We also warn against using photometric redshifts to define environment in all but the densest regions. When considering environment there are two regimes: the ‘local environment’ internal to a halo best measured with nearest neighbour and ‘large-scale environment’ external to a halo best measured with apertures. This leads to the conclusion that there is no universal environment measure and the most suitable method depends on the scale being probed.
Current update on the protective effect of epicatechin in neurodegenerative diseases

1 School of Pharmacy, Suresh Gyan Vihar University, Mahal Road, Jagatpura 302017, Jaipur, India 2 Department of Pharmacology, Saveetha Dental College, Saveetha Institute of Medical and Technical Sciences, Saveetha University, Chennai, India 3 Uttaranchal Institute of Pharmaceutical Sciences, Uttaranchal University, Dehradun, India 4 Department of Pharmacology, College of Pharmacy, Umm Al-Qura University, Makkah, Saudi Arabia 5 Inva-Health Inc, Cranbury, NJ 08512, USA 6 School of Pharmaceutical Sciences, Lovely Professional University, Phagwara, Punjab, 144411, India 7 Faculty of Health, Australian Research Centre in Complementary and Integrative Medicine, University of Technology Sydney, Ultimo, NSW 2007, Australia 8 Discipline of Pharmacy, Graduate School of Health, University of Technology Sydney, NSW 2007, Australia 9 Department of Pharmacology, Maharishi Arvind College of Pharmacy, Ambabari Circle, Ambabari, Jaipur, 302023, India
GEMINI LONG-SLIT OBSERVATIONS OF LUMINOUS OBSCURED QUASARS: FURTHER EVIDENCE FOR AN UPPER LIMIT ON THE SIZE OF THE NARROW-LINE REGION

We examine the spatial extent of the narrow-line regions (NLRs) of a sample of 30 luminous obscured quasars at 0.4 < z < 0.7 observed with spatially resolved Gemini-N GMOS long-slit spectroscopy. Using the [O iii] λ5007 emission feature, we estimate the size of the NLR using a cosmology-independent measurement: the radius where the surface brightness falls to 10−15 erg s−1 cm−2 arcsec−2. We then explore the effects of atmospheric seeing on NLR size measurements and conclude that direct measurements of the NLR size from observed profiles are too large by 0.1–0.2 dex on average, as compared to measurements made to best-fit Sérsic or Voigt profiles convolved with the seeing. These data, which span a full order of magnitude in IR luminosity (log (L8 μm/erg s−1) = 44.4–45.4), also provide strong evidence that there is a flattening of the relationship between NLR size and active galactic nucleus luminosity at a seeing-corrected size of ∼7 kpc. The objects in this sample have high luminosities which place them in a previously under-explored portion of the size–luminosity relationship. These results support the existence of a maximal size of the NLR around luminous quasars; beyond this size, there is either not enough gas or the gas is over-ionized and does not produce enough [O iii] λ5007 emission.
Handbook of prompt gamma activation analysis with neutron beams

Part A: Principles, Techniques and Applications of PGAA. 1. Principles Of The PGAA Method G.L. Molnar. 2. Neutron Beams R.M. Lindstrom. 3. Samples And Standards R.M. Lindstrom. 4. Gamma-Ray Spectrometry T. Belgya. 5. Quantitative Multielement Analysis C. Yonezawa. 6. Applications Of PGAA With Beams D.L. Anderson. Part B: Prompt Gamma-Ray Spectrum Catalogue Zs. Revay, R.B. Firestone. Appendix: Tables Of Atomic And Nuclear Data R.B. Firestone.
Effects of the U$_\textrm{Y}$(1) Chern-Simons term and its baryonic contribution on matter asymmetries and hypermagnetic fields

In this paper, we study the significance of the U$_\textrm{Y}$(1) Chern-Simons term in general, and its baryonic contribution in particular, for the evolution of the matter asymmetries and the hypermagnetic field in the temperature range $100$GeV$\leq T \leq 10$TeV. We show that an initial helical hypermagnetic field, denoted by $B_Y^{(0)}$, can grow matter asymmetries from zero initial value. However, the growth which is initially quadratic with respect to $B_Y^{(0)}$, saturates for values larger than a critical value. The inclusion of the baryonic contribution reduces this critical value, leading to smaller final matter asymmetries. Meanwhile, $B_Y(T_{EW})$ becomes slightly larger than $B_Y^{(0)}$. In the absence of the U$_\textrm{Y}$(1) Chern-Simons term, the final values of matter asymmetries grow without saturation. Conversely, we show that an initial matter asymmetry can grow an initial seed of hypermagnetic field, provided the Chern-Simons term is taken into account. The growth process saturates when the matter asymmetry drops abruptly. When the baryonic contribution is included, the saturation occurs at an earlier time, and $B_Y (T_{EW})$ becomes larger. We also show the results can be within the acceptable range of present day data, provided the inverse cascade process is also taken into account.
Recoil Effects in Microwave Ramsey Spectroscopy

We present a theory of recoil effects in two zone Ramsey spectroscopy, particularly adapted to microwave frequency standards using laser cooled atoms. We describe the atoms by a statistical distribution of Gaussian wave packets which enables us to derive and quantify effects that are related to the coherence properties of the atomic source and that have not been considered previously. We show that, depending on the experimental conditions, the expected recoil frequency shift can be partially cancelled by these effects which can be significant at microwave wavelengths whilst negligible at optical ones. We derive analytical expressions for the observed interference signal in the weak field approximation, and numerical results for realistic caesium fountain parameters. In the near future Cs and Rb fountain clocks are expected to reach uncertainties which are of the same order of magnitude (10^{-16}) as first estimates of the recoil shift at microwave frequencies. We show, however, that the partial cancellation predicted by the complete theory presented here leads to frequency shifts which are up to an order of magnitude smaller. Nonetheless observation of the microwave recoil shift should be possible under particular experimental conditions (increased microwave power, variation of atomic temperature and launching height etc.). We hope that the present paper can provide some guidance for such experiments that would test the underlying theory and its assumptions, which in turn is essential for the next generation of microwave frequency standards.
MINIMAX NONPARAMETRIC PREDICTION UNDER RANDOM SAMPLE SIZE

Let U0 be a random vector taking its values in a measurable space and having an unknown distribution P . Let U1; U2; : : : ; UN and V1; V2; : : : ; Vm be independent simple random samples from P of a random size N and a xed size m, respectively. Further, let z1; z2; : : : ; zk be real valued bounded functions de ned on the same space. Assuming that only the rst sample is observed, we nd a minimax predictor d (N;U1; : : : ; UN ) of the vector Y m = Pm j=1(z1(Vj); z2(Vj); : : : ; zk(Vj)) T with respect to a quadratic error loss function.
THE COUPLED PHYSICAL STRUCTURE OF GAS AND DUST IN THE IM Lup PROTOPLANETARY DISK

The spatial distribution of gas and solids in protoplanetary disks determines the composition and formation efficiency of planetary systems. A number of disks show starkly different distributions for the gas and small grains compared to millimeter–centimeter-sized dust. We present new Atacama Large Millimeter/Submillimeter Array observations of the dust continuum, CO, 13CO, and C18O in the IM Lup protoplanetary disk, one of the first systems where this dust–gas dichotomy was clearly seen. The 12CO is detected out to a radius of 970 au, while the millimeter continuum emission is truncated at just 313 au. Based upon these data, we have built a comprehensive physical and chemical model for the disk structure, which takes into account the complex, coupled nature of the gas and dust and the interplay between the local and external environment. We constrain the distributions of gas and dust, the gas temperatures, the CO abundances, the CO optical depths, and the incident external radiation field. We find that the reduction/removal of dust from the outer disk exposes this region to higher stellar and external radiation and decreases the rate of freeze-out, allowing CO to remain in the gas out to large radial distances. We estimate a gas-phase CO abundance of 5% of the interstellar medium value and a low external radiation field (G0 ≲ 4). The latter is consistent with that expected from the local stellar population. We additionally find tentative evidence for ring-like continuum substructure, suggestions of isotope-selective photodissociation, and a diffuse gas halo.
Analysis of ITER Upper Port Diagnostic First Walls

The Diagnostic First Walls (DFWs) were designed to handle the plasma nuclear and radiant heating along with electro-magnetic loading induced from plasma disruptions. The DFWs also provide custom viewing apertures for the diagnostics within. Consequently, the DFWs contain numerous complex water cooling channels and are designed per ITER SDC-IC for design by analysis. This paper presents the analyses of the Upper Port DFWs proceeding to a final design review. The finite element analyses (FEAs) performed include neutronics, radiative heating, coupled fluid dynamics and heat transfer, and static and transient structural analysis using the combined multi-physics load conditions. Static structural FEAs performed account for the dynamic amplification effects of the transient load. A detailed bolt analysis was also performed per the ITER SDC-IC bolt evaluation based on reaction loads obtained from the mechanical simulations.
Emotional Stress Experience of Care Professionals for Older Adults with Dementia: A Qualitative Interpretive Meta-synthesis

ABSTRACT Emotional stress is a common problem for many professionals in dementia care. Although a plethora of quantitative studies have examined the factors that affect care professionals’ emotional stress, little qualitative research has provided in-depth understanding of professional stress experiences. To magnify the voices of professionals who share their experiences of stress in caring for older adults with dementia, a qualitative interpretive meta-synthesis of five qualitative studies was conducted. Guided by Pearlin’s stress process model, four themes were identified: (1) emotional attachments to older adults with dementia; (2) difficulties in dementia care; (3) stressful working environment; and (4) conflicts with family members of older adults with dementia. Findings further highlighted that professionals’ genuine concern for the well-being of older adults with dementia reinforced the perception of stressors identified in each of the preceding themes. These results could inform the improvements of emotional support for care professionals in practice and policy arenas.
Obesity and acute stress modulate appetite and neural responses in food word reactivity task

Obesity can result from excess intake in response to environmental food cues, and stress can drive greater intake and body weight. We used a novel fMRI task to explore how obesity and stress influenced appetitive responses to relatively minimal food cues (words representing food items, presented similarly to a chalkboard menu). Twenty-nine adults (16F, 13M), 17 of whom had obesity and 12 of whom were lean, completed two fMRI scans, one following a combined social and physiological stressor and the other following a control task. A food word reactivity task assessed subjective food approach (wanting) as well as food avoidant (restraint) responses, along with neural responses, to words denoting high energy-density (ED) foods, low-ED foods, and non-foods. A multi-item ad-libitum meal followed each scan. The obese and lean groups demonstrated differences as well as similarities in activation of appetitive and attention/self-regulation systems in response to food vs. non-food, and to high-ED vs. low-ED food words. Patterns of activation were largely similar across stress and non-stress conditions, with some evidence for differences between conditions within both obese and lean groups. The obese group ate more than the lean group in both conditions. Our results suggest that neural responses to minimal food cues in stressed and non-stressed states may contribute to excess consumption and adiposity.
The driver’s instantaneous situation awareness when the alarm rings during the take-over of vehicle control in automated driving

Abstract Objective The driver’s instantaneous situation awareness in the process of take-over of vehicle control in automated driving has not yet been thoroughly investigated. The proposed research can provide a better understanding of the driver’s perceived characteristics and identify the most urgent information requirements of the on-site scenario when the driver’s eye sight returns from other distractors to the driving scene. Methods We conducted an experiment in simulated automated driving to study the participants’ ability of instantaneous hazard perception and judgment. The scene pictures, which were displayed in millisecond time, were used to imitate the situations that drivers would see when the distracted drivers returned their gaze from the distractive sources to the road in the simulated automated driving. Results The results show that the driving state, scene representation time and hazard levels affect the instantaneous situation awareness of drivers. In addition, the scene perception accuracy of the group who played games during automated driving is much lower than that of the group that chatted with the copilot. The longer picture-showing duration decreases the accuracy of hazard identification, whereas the shorter picture-showing duration increases the accuracy of hazard perception and the hazard rating score. Conclusions In conclusion, distraction reduces the accuracy of the instantaneous scene perception of drivers, and drivers behave more cautiously in decision making when the driving situations are more hazardous. This study provides a good theoretical basis for the design of hazard warning information for automated driving.