Miracle-dz/UniFAR-FTUs huggingface dataset:
Inversion of the geomagnetic induction problem

An algorithm has been found for inverting the problem of geomagnetic induction in a concentrically stratified Earth. It determines the (radial) conductivity distribution from the frequency spectrum of the ratio of internal to external magnetic potentials of any surface harmonic mode. The derivation combines the magnetic induction equation with the principle of causality in the form of an integral constraint on the frequency spectrum. This algorithm generates a single solution for the conductivity. This solution is here proved unique if the conductivity is a bounded, real analytic function with no zeros. Suggestions are made regarding the numerical application of the algorithm to real data.
Lived Experiences of Cebuano LET Topnotchers: A Phenomenological Study

The study was conceptualized to explore the lived experiences of Cebuano LET topnotchers before, during, and after the board exam. The study adopted a hermeneutic phenomenological research design where the in-depth semi-structured interview was made use. Data collected were subjected to thematic analysis and generated the following themes: 1) motivation, (2) multi-factored, (3) highly-individualized preparation, (4) supernatural intervention, (5) discipline, (6) effective test-taking strategies, (7) mixed feelings, and (8) life-changing opportunity. The themes derived to reflect the overall process of becoming a topnotcher and on the transition after becoming one. Their rich experiences would serve as a model and an inspiration for aspiring teachers and topnotchers to come.
Experiences of Transgender Women with Speech Feminization Training: A Qualitative Study

This study investigated the experiences of transgender women after following sessions for speech feminization using semi-structured face-to-face interviews. Transgender women who completed a clinical trial were invited for an interview and 12 accepted the invitation. Interviews were conducted using an interview guide and were recorded and transcribed verbatim. NVivo 12 was used for qualitative data analysis, applying an inductive thematic approach. Four main themes were identified: communication, therapy experiences, impact on mental health, and external factors associated with the outcomes. For most participants, fear of speaking in public decreased after the training and all participants mentioned improved vocal characteristics. Though, reactions ranged from needing more speech therapy to being satisfied with the results. Coping strategies during misgendering occasions differed a lot between participants. More emotive counseling during speech feminization sessions is necessary to help clients in managing possible negative emotions.
Astrocytes in Down Syndrome Across the Lifespan

Down Syndrome (DS) is the most common genetic cause of intellectual disability in which delays and impairments in brain development and function lead to neurological and cognitive phenotypes. Traditionally, a neurocentric approach, focusing on neurons and their connectivity, has been applied to understanding the mechanisms involved in DS brain pathophysiology with an emphasis on how triplication of chromosome 21 leads to alterations in neuronal survival and homeostasis, synaptogenesis, brain circuit development, and neurodegeneration. However, recent studies have drawn attention to the role of non-neuronal cells, especially astrocytes, in DS. Astrocytes comprise a large proportion of cells in the central nervous system (CNS) and are critical for brain development, homeostasis, and function. As triplication of chromosome 21 occurs in all cells in DS (with the exception of mosaic DS), a deeper understanding of the impact of trisomy 21 on astrocytes in DS pathophysiology is warranted and will likely be necessary for determining how specific brain alterations and neurological phenotypes emerge and progress in DS. Here, we review the current understanding of the role of astrocytes in DS, and discuss how specific perturbations in this cell type can impact the brain across the lifespan from early brain development to adult stages. Finally, we highlight how targeting, modifying, and/or correcting specific molecular pathways and properties of astrocytes in DS may provide an effective therapeutic direction given the important role of astrocytes in regulating brain development and function.
The Λ to zero limit of spacetimes and its physical interpretation

We study the behaviour of Schwarzschild–de Sitter spacetime and show, according to Geroch’s notion of spacetime limits, that it converges to the Schwarzschild spacetime. We use an embedding into AdS3 to illustrate and quantify this limiting behaviour. We use these quantitative observations to establish a hierarchy of validity between the Einstein–de Sitter equations and the Einstein equations (and therefore in a weak field limit also Newton’s equations), analogous to the quantum-classical limit when taking .
A Three-Position Spectral Line Survey of Sagittarius B2 between 218 and 263 GHz. II. Data Analysis

We present an analysis of the data from our Swedish-ESO Submillimetre Telescope molecular line survey in the 1.3 mm band of the N, M, and NW positions in the Sgr B2 molecular cloud. The line emissions from 42 molecular species, and some of their isotopomers, were analyzed assuming a single temperature and a homogeneous source. In cases where a source size much smaller than the antenna beam (23″) could be estimated, optical depth effects were also accounted for. In this way rotation temperatures, molecular column densities, and in several cases also source sizes, were determined. Observed and modeled intensities are presented in rotation diagrams. A few complex molecular species, NH2CHO, CH3CHO, C2H3CN, C2H5CN, and CH3OCHO, mainly in the N source, exhibit anomalously strong intensities in their intrinsically weak b- and c-type lines. We argue that this effect can hardly be explained by high optical depths alone, and therefore propose that the possibility of radiative pumping via the low-lying vibrational states of these molecules should be investigated as an alternative explanation. The highest rotation temperatures, up to about 500 K, were found for large molecules toward Sgr B2(N), closely followed by Sgr B2(M). In Sgr B2(NW), which samples the cloud envelope, the rotation temperatures are 15-50 K. For molecules with too few observed transitions to allow determination of rotation temperatures, the column density was calculated assuming optically thin emission, and we adopted rotation temperatures of 50, 50, and 20 K in M, N, and NW, respectively. Column density ratios of isotopomers were determined. After a critical discussion of the resolution-dependent H2 column density toward the observed positions, abundances relative to H2 were calculated. We discuss the chemical differences between the three observed cloud positions and compare with the hot core, compact ridge, and outflow in Orion A. Hot core-type molecules like CH2NH, NH2CN, CH3CN, C2H3CN, and C2H5CN, as well as H2CS, are more abundant in Sgr B2(N) by factors of 3-8 as compared to the M position. Large oxygen-containing species like CH3OH, CH3CHO, CH3OCHO, CH3OCH3, and NH2CHO, of compact ridge-type, show similar or slightly enhanced abundances in N as compared to M. The C2H5OH abundances are similar in N, M, and also in NW. The SO2 and SO abundances in the M core (4 × 10-7 and 1 × 10-7, respectively) are 13 and 5 times higher than in N and are very enhanced (103 and 102 times) as compared to NW. Such high SO2 and SO abundances are also found in the prominent Orion A outflow source. In M the SO18O and S18O data suggest a 16O/18O ratio of 120. The HOCO+ ion is detected in all three positions and appears to be 3 times more abundant in the NW position. HCNH+ is seen only in NW.
Centre shift of the Raman scattered He iiλ 4850 in the symbiotic star V1016 Cygni

We present our spectroscopic data around Hβ of the symbiotic star V 1016 Cyg obtained with the Bohyunsan Echelle Spectrograph, in order to secure the broad emission feature at around λ 4850, which is formed through Raman scattering of Hen λ 972. The total cross-section around Lyy is given approximately by σ(λ) ≃ 1.7 x 10 -28 [λ Lyγ /(λ - 1 Lyγ )] 2 cm 2 , with λ Lyγ being the line centre wavelength of Lyy. We find a centre shift redward by an amount Δλ = +0.64 A in the Raman scattered He II λ 4850. This redward centre shift is exactly analogous to the effect for the Raman scattered He II λ 6545 blueward of Ha discussed in our previous study. We compute the branching ratios of Raman scattering into the level 2s and levels 3s and 3d, which are subsequently incorporated in our Monte Carlo code. Using this code, we present the centre shift of the 4850 feature as a function of the neutral hydrogen column density in the scattering region. Assuming that He II λ 972 emission is characterized by a single Gaussian profile, the redward peak shift observed in the Raman scattered He II λ 4850 feature corresponds to the neutral column density N H1 = 1.2 x 10 21 cm -2 . Assuming that the covering factor ∼0.1 of the scattering region with respect to the He II emission region and adopting a simple spherical stellar wind model, we may place an upper bound M ≤ 3.6 x 10 -7 M ○. yr -1 for the mass-loss rate of the giant component of V1016 Cyg. Our estimate can be severely affected by the kinematics of the scattering and He II emission regions and the exact atomic physics, about which brief discussions are presented.
Why Has U.S. Stock Ownership Doubled Since the Early 1980s? Equity Participation Over the Past Half Century

The U.S. stock ownership rate doubled between 1983 and 2001 but remains below predictions of some equity participation models. Consistent with calibration studies by Heaton and Lucas (2000) and Gomes and Michaelides (2005), mutual fund costs and indicators of background labor risk are significantly related to stock ownership over 19642019. Coefficient estimates and continuous data on driving variables can be used to create a continuous proxy for stock ownership, which could help researchers gauge the effects of shocks that are transmitted via equity participation. Typically omitted asset transfer costs can help analyze other aspects of household portfolio behavior. JEL codes: G11, G02, G23
A New Look at T Tauri Star Forbidden Lines: MHD-driven Winds from the Inner Disk

Magnetohydrodynamic (MHD) and photoevaporative winds are thought to play an important role in the evolution and dispersal of planet-forming disks. We report the first high-resolution (Δv ∼ 6 km s−1) analysis of [S ii] λ4068, [O i] λ5577, and [O i] λ6300 lines from a sample of 48 T Tauri stars. Following Simon et al. we decompose them into three kinematic components: a high-velocity component (HVC) associated with jets, and low-velocity narrow (LVC-NC) and broad (LVC-BC) components. We confirm previous findings that many LVCs are blueshifted by more than 1.5 km s−1 and thus most likely trace a slow disk wind. We further show that the profiles of individual components are similar in the three lines. We find that most LVC-NC and LVC-BC line ratios are explained by thermally excited gas with temperatures between 5000 and 10,000 K and electron densities of ∼107–108 cm−3. The HVC ratios are better reproduced by shock models with a pre-shock H number density of ∼106–107 cm−3. Using these physical properties, we estimate for the LVC and for the HVC. In agreement with previous work, the mass carried out in jets is modest compared to the accretion rate. With the likely assumption that the LVC-NC wind height is larger than the LVC-BC, the LVC-BC is found to be higher than the LVC-NC. These results suggest that most of the mass loss occurs close to the central star, within a few au, through an MHD-driven wind. Depending on the wind height, MHD winds might play a major role in the evolution of the disk mass.
First Detection of a Gravitational Microlensing Candidate toward the Small Magellanic Cloud

We report the first discovery of a gravitational microlensing candidate toward a new population of source stars, the Small Magellanic Cloud (SMC). The candidate event's light curve shows no variation for 3 yr before an upward excursion lasting ~217 days that peaks around 1997 January 11 at a magnification of ~2.1. Microlensing events toward the Large Magellanic Cloud and the Galactic bulge have allowed important conclusions to be reached on the stellar and dark matter content of the Milky Way. The SMC gives a new line of sight through the Milky Way and is expected to prove useful in determining the flattening of the Galactic halo.
Three-dimensional evaluation of maxillary sinus volume following the use of different designs of rapid maxillary expander

Aim of the study: to assess maxillary sinus volume changes (MSV) in adolescent patients with class III malocclusion after application of three types of rapid maxillary expanders (RME). Material and Methods: This was a prospective cohort study that recruited adolescent (13-17 years old) class III malocclusion patients with maxillary deficiency. Patients were randomly assigned to three study groups according to the type of RME: Conventional hyrax (CH), hybrid hyrax (HH), and maxillary skeletal expanders (MSE). Cone-beam computed tomography (CBCT) was used to measure MSV prior to and 6 months after application of RME. Measurements were compared between right and left sides and within study groups. P-values of less than 0.05 were considered significant. Results: A total of 51 patients (30 girls and 21 boys) were included. Mean ages were 14.89±1.6, 15.31±1.73, and 15.59±1.9 Y in the CH, HH and MSE groups respectively. Measurements in all groups were significantly increased. In CH and MSE groups, there was no significant difference between the right and left side before treatment (P =0.386). But in HH, both before and after treatment, the right side values were considerably greater than the left side value (P≤0.05).
Evaporating the Milky Way halo and its satellites with inelastic self-interacting dark matter

Self-interacting dark matter provides a promising alternative for the cold dark matter paradigm to solve potential small-scale galaxy formation problems. Nearly all self-interacting dark matter simulations so far have considered only elastic collisions. Here we present simulations of a galactic halo within a generic inelastic model using a novel numerical implementation in the Arepo code to study arbitrary multi-state inelastic dark matter scenarios. For this model we find that inelastic self-interactions can: (i) create larger subhalo density cores compared to elastic models for the same cross section normalisation; (ii) lower the abundance of satellites without the need for a power spectrum cutoff; (iii) reduce the total halo mass by about 10%; (iv) inject the energy equivalent of O(100) million Type II supernovae in galactic haloes through level de-excitation; (v) avoid the gravothermal catastrophe due to removal of particles from halo centers. We conclude that a ~5 times larger elastic cross section is required to achieve the same central density reduction as the inelastic model. This implies that well-established constraints on self-interacting cross sections have to be revised if inelastic collisions are the dominant mode. In this case significantly smaller cross sections can achieve the same core density reduction thereby increasing the parameter space of allowed models considerably.
Multiwavelength visibility measurements of Miras: observations of R dor and R Leo with MAPPIT

We present interferometric visibility measurements of the nearby Mira-like star R Doradus and the Mira R Leo taken over a wide range of wavelengths (650-990 nm). These are the first simultaneous observations of visibility as a function of wavelength over such a wide wavelength range for a Mira. The observations were made using MAPPIT (Masked APerture-Plane Interference Telescope), an interferometer operating at the 3.9-m Anglo-Australian Telescope. We used a slit to mask the telescope aperture and a prism to disperse the interference pattern in wavelength. We observed in both stars strong decreases in visibility within the TiO absorption bands across the observed wavelength range. Comparison of our results with theoretical models shows general agreement but differences in detail, suggesting that further work is needed to refine the theoretical models. We find that models for stars pulsating in the fundamental mode best fit our observations.
A theoretical model for realistic local climates

We address the question of writing a model that ---considering the doubly-periodic forcing induced by solar radiation and the laws of irradiance and conduction--- reproduces realistic annual and daily modulations of temperatures on the surface of a small region on Earth. The interest in such exercise on theoretical and numeric integration is twofold: the application of this model can give realistic projections of local climate evolution on Earth or on a chosen exoplanet; the creation of such model can shed some light on the effective exchanges of energy among the many actors of this system (atmosphere, water, soil,.). The presence of at least two different thermal reservoirs has as evident consequence the well known phenomenon of lag of seasons, and the less discussed lag of noons (delay in daily temperatures evolution with respect to daily solar radiation). In this article, after describing the motivating phenomena, we develop a physical model, we apply it to many types of climatic zones on Earth, and we compare the results with real temperature data. We finally make some theoretical application to orbits with non zero eccentricity, more in line with actual extra-solar planetary systems.
Dispersive ionospheric Alfvén resonator

A new model of the ionospheric Alfven resonator (IAR) including the effect of wave frequency dispersion is presented. It is shown that the shear Alfven waves in the IAR are coupled to the compressional mode through the boundary conditions at the ionosphere. This coupling results in the appearance of the Hall dispersion and subsequent shift of the IAR frequency spectrum. The excitation mechanism involving the IAR interaction with the magnetospheric convective flow is considered. It is shown that the Hall dispersion of the IAR eigenmode increases the growth rate of the feedback instability. However, for the observed values of ionospheric conductivity this effect is not very high. It is shown that the physical mechanism of the feedback instability is similar to the Cerenkov radiation in collisionless plasmas. The IAR eigenfrequencies and growth rates are evaluated for the case of exponential variation of the Alfven velocity with altitude in the topside ionosphere.
What Do We Really Know about Cosmic Acceleration?

Essentially all of our knowledge of the acceleration history of the universe (even the discovery of the acceleration itself) is predicated on the validity of general relativity through the Friedmann equation. Assuming only a flat spacetime that is homogenous and isotropic on large scales and described by a metric theory of gravity, we use SNe Ia to analyze the acceleration history. We infer robust conclusions about cosmic acceleration that are independent of a particular parameterization of the acceleration history. Specifically, we find (1) very strong (5 σ) evidence for a period of acceleration, (2) strong evidence that the acceleration has not been constant, (3) evidence for an earlier period of deceleration, and (4) only weak evidence that the universe has been accelerating since z ~ 0.3.
Harmonically trapped Bose–Bose mixtures: a quantum Monte Carlo study

We study a harmonically confined Bose–Bose mixture using quantum Monte Carlo methods. Our results for the density profiles are systematically compared with mean-field predictions derived through the Gross–Pitaevskii (GP) equation in the same conditions. The phase space as a function of the interaction strengths and the relation between masses is quite rich. The miscibility criterion for the homogeneous system applies rather well to the system, with some discrepancies close to the critical line for separation. We observe significant differences between the mean-field results and the Monte Carlo ones, that magnify when the asymmetry between masses increases. In the analyzed interaction regime, we observe universality of our results which extend beyond the applicability regime for the GP equation.
Calibration and Limitations of the Mg ii Line-based Black Hole Masses

We present single-epoch black hole mass ( ) calibrations based on the rest-frame ultraviolet (UV) and optical measurements of Mg ii 2798 Å and Hβ 4861 Å lines and the active galactic nucleus (AGN) continuum, using a sample of 52 moderate-luminosity AGNs at z ∼ 0.4 and z ∼ 0.6 with high-quality Keck spectra. We combine this sample with a large number of luminous AGNs from the Sloan Digital Sky Survey to increase the dynamic range for a better comparison of UV and optical velocity and luminosity measurements. With respect to the reference based on the line dispersion of Hβ and continuum luminosity at 5100 Å, we calibrate the UV and optical mass estimators by determining the best-fit values of the coefficients in the mass equation. By investigating whether the UV estimators show a systematic trend with Eddington ratio, FWHM of Hβ, Fe ii strength, or UV/optical slope, we find no significant bias except for the slope. By fitting the systematic difference of Mg ii-based and Hβ-based masses with the L3000/L5100 ratio, we provide a correction term as a function of the spectral index as ΔC = 0.24 (1 + αλ) + 0.17, which can be added to the Mg ii-based mass estimators if the spectral slope can be well determined. The derived UV mass estimators typically show >∼0.2 dex intrinsic scatter with respect to the Hβ-based , suggesting that the UV-based mass has an additional uncertainty of ∼0.2 dex, even if high-quality rest-frame UV spectra are available.
Stellar Populations of Shell Galaxies

We present a study of the inner (out to $\sim$1 R$_{\mathrm{eff}}$) stellar populations of 9 shell galaxies. We derive stellar population parameters from long slit spectra by both analyzing the Lick indices of the galaxies and by fitting Single Stellar Population model spectra to the full galaxy spectra. The results from the two methods agree reasonably well. Many of the shell galaxies in our sample appear to have lower central $\mathrm{Mg}_{2}$ index values than non-shell galaxies of the same central velocity dispersion, which is likely due to a past interaction event. Our shell galaxy sample shows a relation between central metallicity and velocity dispersion that is consistent with previous samples of non-shell galaxies. Analyzing the metallicity gradients in our sample, we find an average metallicity gradient of -0.16$\pm$0.10 dex per decade in radius. We compare this with formation models to constrain the merging history of shell galaxies. We argue that our galaxies likely have undergone major mergers in their past but it is unclear whether the shells formed from these events or from separate minor mergers. Additionally, we find evidence for young stellar populations ranging in age from 500 Myr to 4--5 Gyr in four of the galaxies, allowing us to speculate on the age of the shells. For NGC 5670, we use a simple dynamical model to find the time required to produce the observed distribution of shells to be consistent with the age of the young subpopulation, suggesting that the shells likely formed from the same event that led to the young subpopulation.