Miracle-dz/UniFAR-FTUs huggingface dataset:
Revisiting the physiological role of androgens in women

ABSTRACT Introduction Extensive research underlines the critical functions of androgens in females. Nevertheless, the precise mechanisms of their action are poorly understood. Here, we review the existing literature regarding the physiological role of androgens in women throughout life. Areas covered Several studies show that androgen receptors (ARs) are broadly expressed in numerous female tissues. They are essential for many physiological processes, including reproductive, sexual, cardiovascular, bone, muscle, and brain health. They are also involved in adipose tissue and liver function. Androgen levels change with the menstrual cycle and decrease in the first decades of life, independently of menopause. Expert opinion To date, studies are limited by including small numbers of women, the difficulty of dosing androgens, and their cyclical variations. In particular, whether androgens play any significant role in regulating the establishment of pregnancy is poorly understood. The neural functions of ARs have also been investigated less thoroughly, although it is expressed at high levels in brain structures. Moreover, the mechanism underlying the decline of dehydroepiandrosterone (DHEA) and dehydroepiandrosterone sulfate (DHEAS) with age is unclear. Other factors, including estrogen’s effect on adrenal androgen production, reciprocal regulation of ARs, and non-classical effects of androgens, remain to be determined.
EVIDENCE FOR SLOW MIGRATION OF NEPTUNE FROM THE INCLINATION DISTRIBUTION OF KUIPER BELT OBJECTS

Much of the dynamical structure of the Kuiper Belt can be explained if Neptune migrated over several AU, and/or if Neptune was scattered to an eccentric orbit during planetary instability. An outstanding problem with the existing formation models is that the distribution of orbital inclinations they predicted is narrower than the one inferred from observations. Here we perform numerical simulations of Kuiper Belt formation starting from an initial state with Neptune at 20 < a N , 0 < 30 ? > AU and a dynamically cold outer disk extending from beyond a N , 0 ? > to 30 AU. Neptune’s orbit is migrated into the disk on an e-folding timescale 1 ≤ τ ≤ 100 Myr. A small fraction (∼10−3) of the disk planetesimals become implanted into the Kuiper belt in the simulations. By analyzing the orbital distribution of the implanted bodies in different cases we find that the inclination constraint implies that τ ≳ 10 ? > Myr and a N , 0 ≲ 25 ? > AU. The models with τ < 10 ? > Myr do not satisfy the inclination constraint, because there is not enough time for various dynamical processes to raise inclinations. The slow migration of Neptune is consistent with other Kuiper Belt constraints, and with recently developed models of planetary instability/migration. Neptune’s eccentricity and inclination are never large in these models ( e N < 0.1 ? > , i N < 2 ° ? > ), as required to avoid excessive orbital excitation in the >40 AU region, where the Cold Classicals presumably formed.
Novel gluino cascade decays in $E_6$ inspired models

We point out that the extra neutralinos and charginos, generically appearing in a large class of $E_6$ inspired models, lead to distinctive signatures from gluino cascade decays involving longer decay chains, more visible transverse energy, softer jets and leptons and less missing transverse energy than in the Minimal Supersymmetric Standard Model (MSSM). On the one hand, this makes the gluino harder to discover for certain types of conventional analysis. On the other hand, the $E_6$ inspired models have enhanced 3- and 4-lepton signatures, as compared to the MSSM, making the gluino more visible in these channels. After extensive scans over the parameter space, we focus on representative benchmark points for the two models, and perform a detailed Monte Carlo analysis of the 3-lepton channel, showing that $E_6$ inspired models are clearly distinguishable from the MSSM in gluino cascade decays.
The dynamical evolution of molecular clouds near the Galactic Centre – II. Spatial structure and kinematics of simulated clouds

The evolution of molecular clouds in galactic centres is thought to differ from that in galactic discs due to a significant influence of the external gravitational potential. We present a set of numerical simulations of molecular clouds orbiting on the 100-pc stream of the Central Molecular Zone (the central $\sim500$ pc of the Galaxy) and characterise their morphological and kinematic evolution in response to the background potential and eccentric orbital motion. We find that the clouds are shaped by strong shear and torques, by tidal and geometric deformation, and by their passage through the orbital pericentre. Within our simulations, these mechanisms control cloud sizes, aspect ratios, position angles, filamentary structure, column densities, velocity dispersions, line-of-sight velocity gradients, spin angular momenta, and kinematic complexity. By comparing these predictions to observations of clouds on the Galactic Centre 'dust ridge', we find that our simulations naturally reproduce a broad range of key observed morphological and kinematic features, which can be explained in terms of well-understood physical mechanisms. We argue that the accretion of gas clouds onto the central regions of galaxies, where the rotation curve turns over and the tidal field is fully compressive, is accompanied by transformative dynamical changes to the clouds, leading to collapse and star formation. This can generate an evolutionary progression of cloud collapse with a common starting point, which either marks the time of accretion onto the tidally-compressive region or of the most recent pericentre passage. Together, these processes may naturally produce the synchronised starbursts observed in numerous (extra)galactic nuclei.
Induced diffusion of tracers in a bacterial suspension: theory and experiments

Abstract The induced diffusion of tracers in a bacterial suspension is studied theoretically and experimentally at low bacterial concentrations. Considering the swimmer–tracer hydrodynamic interactions at low Reynolds number and using a kinetic theory approach, it is shown that the induced diffusion coefficient is proportional to the swimmer concentration, their mean velocity and a coefficient $\beta $ , as observed experimentally. This paper shows that $\beta $ increases as a result of the interaction with solid surfaces. The coefficient $\beta $ scales as the tracer–swimmer cross-section times the mean square displacement produced by single scattering events, which depends on the swimmer propulsion forces. Considering simple swimmer models (acting on the fluid as two monopoles or as a force dipole), it is shown that $\beta $ increases for decreasing swimming efficiencies. Close to solid surfaces, the swimming efficiency degrades and, consequently, the induced diffusion increases. Experiments on wild-type Escherichia coli in a Hele-Shaw cell, under buoyant conditions, are performed to measure the induced diffusion on tracers near surfaces. The modification of the suspension pH varies the swimmers’ velocity over a wide range, allowing the $\beta $ coefficient to be extracted with precision. It is found that solid surfaces modify the induced diffusion: decreasing the confinement height of the cell, $\beta $ increases by a factor of 4. The theoretical model reproduces this increase, although there are quantitative differences, probably attributed to the simplicity of the swimmer models and to the estimates for the parameters that model E. coli.
Morphology and Distribution of Thermo- Hygro-Ir- and Chemo-Receptors for Females of Family Diaspididae (Hemiptera: Sternorrhyncha)

The comparative study of the female body structures of many species of Diaspididae has been done using Leica microsystems. Several types of sensilla were described for three species namely: Parlatoria zizyphii , Lepidosaphes ficus and Lepidosaphes beckii . Four thermo-hygro-sensory species as sensing organs for temperature and humidity, namely plachodea in lepidosaphes beckii , sensilla basiconica and styloconica in Parlatoria zizyphii , sensilla caeloconica in lepidosaphes ficus and tuft organ in lepidosaphes ficus ; One type of gustatory receptor is a styloconica in Parlatoria zizyphii ; infrared receptors (IR), also in Parlatoria zizyphii ; olfactory organs such as sensilla placodea in Parlatoria zizyphii. Measurements of sense organs in different species were done using ocular micrometer. Also, dimension measurements of each sensillum of temporary and permanent females mounts were done. According to these comparative studies, the general regulation of sensilla was assumed to be Diaspididae. Eight sensory phenotypes were identified, with an attempt to use these data at the systemic level. The results of this study provide an important basis for linking morphological characteristics of sensory organs to insect behavior and should stimulate the development of effective quasi-chemistry-based control strategies against species belonging to the
Effect of Irradiation with 980-nm Diode Laser on the Microhardness of Young and Old Root Canal Dentin after Treatment with Chemical Solutions

Purpose: The purpose of this study was to evaluate the effect of diode laser-980nm on microhardness of young and old canal dentin after treatment with NaOCl, NaOCl/ EDTA and distilled water solutions. Material and Methods Forty-eight single rooted premolars were divided into three groups according to the chemical solutions used (16 each) (8 for young teeth <30 years old and 8 for old teeth >50 years old). Group I: irrigated with 5ml of 2.6% NaOCl activated with diode laser, group II: irrigated with 5ml of 2.6% NaOCl without laser activation followed by 5ml of 17% EDTA activated with diode laser and group III: irrigated with 5ml of distilled water activated with diode laser. Then microhardness was evaluated at coronal, middle, and apical thirds of each root canal. Results: In all young and old groups, the coronal third had the highest mean value, followed by the middle, and the apical third had the lowest mean value, with a statistically significant difference between thirds of the groups ( p 0.001<). There was a statistically significant difference between young and old teeth at all levels (coronal, middle, and apical) for each group (I, II, and III), with old teeth having a greater mean microhardness value than young teeth. Conclusion: Irradiation of NaOCl/EDTA solutions with 980-nm diode caused reduction in microhardness of young dentin more than old dentin, and NaOCl only or distilled water in all thirds of groups.
Energetic constraints to chemo-photometric evolution of spiral galaxies

The problem of chemo-photometric evolution of late-type galaxies is dealt with relying on prime physical arguments of energetic self-consistency between chemical enhancement of galaxy mass, through nuclear processing inside stars, and luminosity evolution of the system. Our analysis makes use of the Buzzoni template galaxy models along the Hubble morphological sequence. The contribution of Type II and Ia SNe is also accounted for in our scenario. Chemical enhancement is assessed in terms of the so-called ‘yield metallicity’ ( Z ), that is the metal abundance of processed mass inside stars, as constrained by the galaxy photometric history. For a Salpeter initial mass function (IMF), Z ∝ t 0 . 23 being nearly insensitive to the galaxy star formation history. The interstellar medium (ISM) metallicity can be set in terms of Z , and just modulated by the gas fraction and the net fraction of returned stellar mass ( f ). For the latter, a safe upper limit can be placed, such as f (cid:2) 0.3 at any age. The comparison with the observed age–metallicity relation allows us to set a ﬁrm upper limit to the Galaxy birthrate, such as b (cid:2) 0.5, and to the chemical enrichment ratio (cid:3) Y / (cid:3) Z (cid:2) 5. About four out of ﬁve stars in the solar vicinity are found to match the expected Z ﬁgure within a factor of 2, a feature that leads us to conclude that star formation in the Galaxy must have proceeded, all the time, in a highly contaminated environment where returned stellar mass is in fact the prevailing component to gas density. relationships, as suggested by the observations. Namely (i) the down-sizing mechanism appears to govern star formation in the local Universe; (ii) the ‘delayed’ star formation among low-mass galaxies, as implied by the inverse b − M gal dependence, naturally leads to a more copious gas fraction when moving from giant to dwarf galaxies; (iii) although lower-mass galaxies tend more likely to take the look of later-type spirals, it is mass, not morphology, that drives galaxy chemical properties. Facing the relatively ﬂat trend of Z versus galaxy type, the increasingly poorer gas metallicity, as traced by the [O/H] abundance of H II regions along the Sa → Im Hubble sequence, seems to be mainly the result of the softening process, that dilute enriched stellar mass within a larger fraction of residual gas. The problem of the residual lifetime for spiral galaxies as active star-forming systems has been investigated. If returned mass is left as the main (or unique) gas supplier to the ISM, as implied by the Roberts time-scale, then star formation might continue only at a maximum birthrate b max (cid:4) f /(1 − f ) (cid:2) 0.45, for a Salpeter IMF. As a result, only massive ( M gal (cid:3) 10 11 M (cid:5) ) Sa/Sb spirals may have some chance to survive ∼ 30 per cent or more beyond a Hubble time. Things may be worse, on the contrary, for dwarf systems, that seem currently on the verge of ceasing their star formation activity unless to drastically reduce their apparent birthrate below the b max threshold.
Partition Functions of $\mathcal{N}=1$ Gauge Theories on $S^2 \times \mathbb{R}^2_\varepsilon$ and Duality

We compute the partition functions of $\mathcal{N} = 1$ gauge theories on $S^2 \times \mathbb{R}^2_\varepsilon$ using supersymmetric localization. The path integral reduces to a sum over vortices at the poles of $S^2$ and at the origin of $\mathbb{R}^2_\varepsilon$. The exact partition functions allow us to test Seiberg duality beyond the supersymmetric index. We propose the $\mathcal{N} = 1$ partition functions on the $\Omega$-background, and show that the Nekrasov partition functions can be recovered from these building blocks.
Who is Truly a Person with High Self-Regulation? One Who “does the Task They Dislike First” or Who “Eats the Food They Dislike First”?

The purpose of this study was to clarify what personality trait determines task order. We conducted a web survey (N=224, 126 men and 98 women, 20-72 years age). We asked about task order in two different decision-making situations, and measured personality traits: self-regulation, BIS, and BAS. The results showed that people who start by first doing tasks they dislike had more self-regulation. For eating situations, the results indicated that people who first eat food they dislike had more self-regulation based on an automatic motivational system. Therefore, task order may involve self-regulation of different properties. In future studies, it will be necessary to approach task order from the perspective of different self-regulation: automatic self-regulation and executive function control.
Social Network Analysis of the Adoption of an Agricultural Innovation in a Village in Assiut Governorate

: This research endeavors to know about the network characteristics of the respondents' farmers inside an innovation adoption network, and to identify the relationship between their network characteristics and the time of adoption of this innovation. Data were collected from all farmers of one of the villages of Assiut governorate by questionnaire. The study used UCINET software to analyze and visualize the data. The results identified the farmers with the best network characteristics among farmers in the whole network. Social network analysis states that we can rely on them to convince the largest number of farmers to adopt the innovation very rapidly with the shortest links. Also it cleared up that there's a positive significance correlation between the time of adoption of the innovation and these variables: degree of reach, out-geodesic distances and efficiency of ego network. On the other hand, it came to clear that there's a negative significance correlation between the time of adoption of the innovation and these variables: number of directed ties, density of ego network, two-step reach and closeness centrality.
Performance Analysis of Dihedral Corner Reflectors for Slope Movements: A Case Study From Aniangzhai Landslide in China

Using synthetic aperture radar (SAR) and interferometric SAR (InSAR) technology, artificial corner reflectors (CRs) are popular coherent targets for monitoring ground instability with subcentimeter accuracy in nonurban areas. In this letter, we investigate the performance of a newly designed small dihedral CR for monitoring postfailure creep at the Aniangzhai landslide in Danba County, China. The new double geometry CRs consist of two sets of semicircular metal plates, each 30–40 cm in radius and perpendicular to each other. Six such CRs are installed for CR-InSAR analysis using both TerraSAR-X (TSX) high-resolution spotlight (HS) data and medium-resolution Sentinel-1 (S1) SAR images. The CRs are first identified in SAR images using a probability model by taking into three factors. These are: 1) inverse of amplitude dispersion; 2) intensity increment after the installation; and 3) an upper empirical bound derived from the ensemble average of pixel intensities in postdeployment SAR images. Experimental results show that the CRs improve the background intensity in TSX images by around 30 dB, with signal-to-clutter ratio (SCR) exceeding 25 dB. Furthermore, the radar cross section (RCS) of CRs in both TSX and S1 images remains relatively stable, ranging from 15 to 23 dB, making them suitable for CR-InSAR analysis using double-difference phase observations.
On the fermionic frequencies of circular strings

We revisit the semiclassical computation of the fluctuation spectrum around different circular string solutions in AdS5 × S5 and , starting from the Green–Schwarz action. It has been known that the results for these frequencies obtained from the algebraic curve and from the worldsheet computations sometimes do not agree. In particular, different methods give different results for the half-integer shifts in the mode numbers of the frequencies. We find that these discrepancies can be removed if one carefully takes into account the transition matrices in the spin bundle over the target space.
Extreme quasars at high redshift

Context. Quasars radiating at extreme Eddington ratios (hereafter xA quasars) are likely a prime mover of galactic evolution and have been hailed as potential distance indicators. Their properties are still scarcely known. Aims. We aim to test the effectiveness of the selection criteria defined on the “4D Eigenvector 1” (4DE1) for identifying xA sources. We provide a quantitative description of their rest-frame UV spectra (1300–2200 Å) in the redshift range 2 ≲ z ≲ 2.9, with a focus on major emission features. Methods. Nineteen extreme quasar candidates were identified using 4DE1 selection criteria applied to SDSS spectra: Al IIIλ1860Si IIIλ1892 ≳0.5 and C IIIλ1909/Si IIIλ1892 ≲1. The emission line spectra was studied using multicomponent fits of deep spectroscopic observations (S/N ≳ 40 − 50; spectral resolution ≈250 km s−1) obtained with the OSIRIS at Gran Telescopio Canarias (GTC). Results. GTC spectra confirm that almost all of these quasars are xA sources with very similar properties. We provide spectrophotometric and line profile measurements for the Si IVλ1397+O IV, C IVλ1549+He IIλ1640, and the 1900 Å blend. This last feature is found to be predominantly composed of Al IIIλ1860, Si IIIλ1892 and Fe III emission features, with weak C IIIλ1909. The spectra can be characterized as very low ionization (ionization parameter, logU ∼ −3), a condition that explains the significant Fe III emission observed in the spectra. xA quasars show extreme properties in terms of C IVλ1549 equivalent width and blueshift amplitudes. C IVλ1549 shows low equivalent width, with a median value of 15 Å (≲30 Å for the most sources), and high or extreme blueshift amplitudes (–5000 ≲ c(1/2) ≲ –1000 km s−1). Weak-lined quasars appear as extreme xA quasars and not as an independent class. The C IVλ1549 high amplitude blueshifts coexists in all cases save one with symmetric and narrower Al IIIλ1860 and Si IIIλ1892 profiles. Estimates of the Eddington ratio using the Al IIIλ1860 FWHM as a virial broadening estimator are consistent with the ones of a previous xA sample. Conclusions. xA quasars show distinguishing properties that make them easily identifiable in large surveys and potential “standard candles” for cosmological applications. It is now feasible to assemble large samples of xA quasars from the latest data releases of the SDSS. We provide evidence that Al IIIλ1860 could be associated with a low-ionization virialized subsystem, supporting previous suggestions that Al III is a reliable virial broadening estimator.
Universal Linear Scaling of Topological Phase Transition in Band Theory

We develop a unified view of topological phase transitions (TPTs) in solids by revising the classical band theory with the inclusion of topology. Taking the TPT between normal insulators (NIs) and quantum spin Hall (QSH) insulators as an example, we demonstrate that the critical transition point is underlined by a universal linear scaling between the characteristic bond strength and average bond length. The validity of this scaling relation is verified in various two-dimensional (2D) systems including crystalline, quasicrystalline and amorphous lattices based on a generic tight-binding model. Furthermore, this universal linear scaling is shown to set an upper bound for the degree of structural disorder to destroy the topological order in a crystalline solid, as exemplified by formation of vacancies and thermal disorder. Our work formulates a simple framework for understanding the physical nature of 2D TPTs with significant implications in practical applications of topological materials.
INTEGRATED NUCLEOSYNTHESIS IN NEUTRINO-DRIVEN WINDS

Although they are but a small fraction of the mass ejected in core-collapse supernovae, neutrino-driven winds (NDWs) from nascent proto-neutron stars (PNSs) have the potential to contribute significantly to supernova nucleosynthesis. In previous works, the NDW has been implicated as a possible source of r-process and light p-process isotopes. In this paper, we present time-dependent hydrodynamic calculations of nucleosynthesis in the NDW which include accurate weak interaction physics coupled to a full nuclear reaction network. Using two published models of PNS neutrino luminosities, we predict the contribution of the NDW to the integrated nucleosynthetic yield of the entire supernova. For the neutrino luminosity histories considered, no true r-process occurs in the most basic scenario. The wind driven from an older 1.4 M☉ model for a PNS is moderately neutron-rich at late times however, and produces 87Rb, 88Sr, 89Y, and 90Zr in near solar proportions relative to oxygen. The wind from a more recently studied 1.27 M☉ PNS is proton-rich throughout its entire evolution and does not contribute significantly to the abundance of any element. It thus seems very unlikely that the simplest model of the NDW can produce the r-process. At most, it contributes to the production of the N = 50 closed shell elements and some light p-nuclei. In doing so, it may have left a distinctive signature on the abundances in metal-poor stars, but the results are sensitive to both uncertain models for the explosion and the masses of the neutron stars involved.