Miracle-dz/UniFAR-FTUs huggingface dataset:
Undergraduate Student Perceptions of Industry Guest Speakers in the College Classroom

The use of guest speakers in college classes is a well-accepted pedagogical practice, but the academic literature has generally been based on instructor or event organizers’ anecdotal reflections about particular experiences. Moreover, research based upon students’ considerations of this practice have been especially sparse. The purpose of this study is to explore student perceptions of guest speakers to determine what value students find in them. One-hundred fourteen students participated in a qualitative survey, answering questions about their prior experiences with and expectations of industry guest speakers. The results showed that 86.1% of respondents who had previously been enrolled in a college class that featured an industry guest speaker visit liked the experience, especially if the guest currently worked in a field related to course content, spoke enthusiastically and honestly, and answered questions. In particular, participants appreciated hearing insider information about the speaker’s day-to-day work life, as well as advice for their own career path. Recommendations are provided to university educators as guidance for improving student experiences and engagement with guest speakers, especially those from the fashion industry.
Chemical tracers of high-metallicity environments

We present for the first time a detailed study of the properties of molecular gas in metal-rich environments such as early-type galaxies (ETGs). We have explored photon-dominated region chemistry for a wide range of physical conditions likely to be appropriate for these sources. We derive fractional abundances of the 20 most chemically reactive species as a function of the metallicity, as a function of the optical depth and for various volume number gas densities, far-ultraviolet (FUV) radiation fields and cosmic ray ionization rates. We also investigate the response of the chemistry to the changes in α-element enhancement as seen in ETGs. We find that the fractional abundances of CS, H2S, H2CS, H2O, H3O+, HCO+ and H2CN seem invariant to an increase of metallicity whereas C+, CO, C2H, CN, HCN, HNC and OCS appear to be the species most sensitive to this change. The most sensitive species to the change in the fractional abundance of α-elements are C+, C, CN, HCN, HNC, SO, SO2, H2O and CS. Finally, we provide line brightness ratios for the most abundant species, especially in the range observable with Atacama Large Millimeter Array (ALMA). Discussion of favourable line ratios to be used for the estimation of supersolar metallicities and α-elements are also provided.
Future Direct Spectroscopic Detection of Hot Jupiters with IGRINS

With about 700 confirmed extrasolar planets, it is time to move beyond discovery and towards characterization. Perhaps the most basic parameter of an extrasolar planet is its mass; however, this is very difficult to determine if the planet does not transit the star. The radial velocity technique, still the most fruitful method of discovering planets in the solar neighborhood, can only determine a minimum planet mass. We investigate a method using the near-future IGRINS near infrared spectrograph to detect the orbital motion of the planet itself. We simulate several observations of a star with an orbiting planet, and search for the spectral signature of the planet by cross-correlating against planet model spectra. A detection appears as a strong peak in the cross-correlation function, and gives the radial velocity of the planet at the time of observation. This, combined with the motion of the star from traditional radial velocity planet search programs, can determine the actual planet mass. We find that the IGRINS instrument can detect the spectral signature from large planets on very close orbits (so-called Hot Jupiters), and that the detections can provide tight constraints on the true planet mass.
Detectability of torsion gravity via galaxy clustering and cosmic shear measurements

Alterations of the gravity Lagrangian introduced in modified torsion gravity theories---also referred to as $f(T)$ gravity---allows for an accelerated expansion in a matter dominated Universe. In this framework, the cosmic speed up is driven by an effective `torsion fluid'. Besides the background evolution of the Universe, structure formation is also modified because of a time dependent effective gravitational constant. Here, we investigate the imprints of $f(T)$ gravity on galaxy clustering and weak gravitational lensing to the aim of understanding whether future galaxy surveys could constrain torsion gravity and discriminate amongst it and standard general relativity. Specifically, we compute Fisher matrix forecasts for two viable $f(T)$ models to both infer the accuracy on the measurement of the model parameters and evaluate the power that a combined clustering and shear analysis will have as a tool for model selection. We find that with such a combination of probes it will indeed be possible to tightly constrain $f(T)$ model parameters. Moreover, the Occam's razor provided by the Bayes factor will allow us to confirm an $f(T)$ power-law extension of the concordance $\Lambda{\rm CDM}$ model, were a value larger than 0.02 of its power-law slope measured, whereas in $\Lambda{\rm CDM}$ it is exactly 0.
Cluster AgeS ExperimentCatalog of variable stars in the globular cluster omega Centauri

We present results of a photometric survey for variable stars in the field of the globular cluster ω Centauri. The observed region was centered roughly on the cluster core and covered 644 arcmin 2 . The cluster was monitored on 59 nights in 1999 and 2000. A total of 117 new variables were identified. Among them there are 17 RR Lyr-type stars, 35 SX Phe variables and 26 eclipsing binaries. A comprehensive catalog including all variable stars so far reported from the cluster field is presented. We list basic photometric properties and provide finding charts for a total of 392 objects. For 313 of them new BV light curves were obtained. The presented sample includes several interesting variables, such as SX Phe stars with extremely short periods of pulsation and several candidates for pulsating K giants. Optical counterparts to 9 X-ray sources detected by XMM and Chandra telescopes were identified: all of them are likely to be foreground variables not related to the cluster.
Risk Based bank rating and financial performance of Indonesian commercial banks with GCG as intervening variable

Abstract This study aims to analyze the effect of the financial health of Indonesian commercial banks on financial performance with good corporate governance as an intervening variable. This study utilizes the risk-based bank rating (RBBR) method with secondary data by examining annual reports of 41 commercial banks taken as samples for the period from 2014 to 2019. The ratios used in this study are Non-Performing Loans (NPL), Loan Deposit Ratio (LDR), Net Interest Margin (NIM), and Operating Efficiency Ratio (OER), Capital Adequacy Ratio (CAR), Return on Assets (ROA) and Good Corporate Governance (GCG). The results showed that NIM had a direct positive and significant effect on ROA, while OER had a negative and significant effect on ROA, as hypothesized. Direct testing of GCG shows a negative and significant effect of NPL and OER, as well as a positive and significant effect of NIM. Furthermore, indirect testing with intervening variables shows that GCG is able to mediate the relationship between NPL and OER on the financial performance of conventional banks in Indonesia. In addition, GCG is also empirically proven to strengthen the positive and significant effect of NIM on ROA. This finding underscores the importance of good corporate governance in improving the financial health of commercial banks in Indonesia. In addition, the results theoretically would imply for the relevance of investigations regarding governance mechanisms and moral ethics as the domains of strategic issues of corporate governance.
OBSERVING EVOLUTION IN THE SUPERGRANULAR NETWORK LENGTH SCALE DURING PERIODS OF LOW SOLAR ACTIVITY

We present the initial results of an observational study into the variation of the dominant length scale of quiet solar emission: supergranulation. The distribution of magnetic elements in the lanes that from the network affects, and reflects, the radiative energy in the plasma of the upper solar chromosphere and transition region at the magnetic network boundaries forming as a result of the relentless interaction of magnetic fields and convective motions of the Suns’ interior. We demonstrate that a net difference of ∼0.5 Mm in the supergranular emission length scale occurs when comparing observation cycle 22/23 and cycle 23/24 minima. This variation in scale is reproduced in the data sets of multiple space- and ground-based instruments and using different diagnostic measures. By means of extension, we consider the variation of the supergranular length scale over multiple solar minima by analyzing a subset of the Mount Wilson Solar Observatory Ca ii K image record. The observations and analysis presented provide a tantalizing look at solar activity in the absence of large-scale flux emergence, offering insight into times of “extreme” solar minimum and general behavior such as the phasing and cross-dependence of different components of the spectral irradiance. Given that the modulation of the supergranular scale imprints itself in variations of the Suns’ spectral irradiance, as well as in the mass and energy transport into the entire outer atmosphere, this preliminary investigation is an important step in understanding the impact of the quiet Sun on the heliospheric system.
STRONG BRIGHTNESS VARIATIONS SIGNAL CLOUDY-TO-CLEAR TRANSITION OF BROWN DWARFS

We report the results of a J-band search for cloud-related variability in the atmospheres of 62 L4–T9 dwarfs using the Du Pont 2.5 m telescope at Las Campanas Observatory and the Canada–France–Hawaii Telescope on Mauna Kea. We find 9 of 57 objects included in our final analysis to be significantly variable with >99% confidence, 5 of which are new discoveries. In our study, strong signals (peak-to-peak amplitudes >2%) are confined to the L/T transition (4/16 objects with L9–T3.5 spectral types and 0/41 objects for all other spectral types). The probability that the observed occurrence rates for strong variability inside and outside the L/T transition originate from the same underlying true occurrence rate is excluded at >99.7% confidence. Based on a careful assessment of our sensitivity to astrophysical signals, we infer that 39% of L9–T3.5 dwarfs are strong variables on rotational timescales. If we consider only L9–T3.5 dwarfs with 0.8 < J − Ks < 1.5, and assume an isotropic distribution of spin axes for our targets, we find that % would be strong variables if viewed edge-on; azimuthal symmetry and/or binarity may account for non-variable objects in this group. These observations suggest that the settling of condensate clouds below the photosphere in brown dwarf (BD) atmospheres does not occur in a spatially uniform manner. Rather, the formation and sedimentation of dust grains at the L/T transition is coupled to atmospheric dynamics, resulting in highly contrasting regions of thick and thin clouds and/or clearings. Outside the L/T transition we identify five weak variables (peak-to-peak amplitudes of 0.6%–1.6%). Excluding L9–T3.5 spectral types, we infer that % of targets vary with amplitudes of 0.5%–1.6%, suggesting that surface heterogeneities are common among L and T dwarfs. Our survey establishes a significant link between strong variability and L/T transition spectral types, providing evidence in support of the hypothesis that cloud holes contribute to the abrupt decline in condensate opacity and 1 μm brightening observed in this regime. More generally, fractional cloud coverage is an important model parameter for BDs and giant planets, especially those with L/T transition spectral types and colors.
A conformally invariant gauge fixing equation and a field strength for the symmetric traceless field over four dimensional conformally flat Einstein spacetimes

The conformally invariant symmetric traceless field $A$ is considered on conformally flat Einstein space-time. If $d=4$ this field possess a scalar gauge invariance. In that case, we provide a conformally invariant gauge condition which generalizes in a simple manner, on those space-time, the Eastwood-Singer gauge condition. A field strength $F$ is built upon the potential $A$, its properties are worked out in details, giving raise to a new set of conformally invariant equations.
Predictor Prognosis of Pediatric Septic Shock : Literature review

Introduction: The unpredictability of body response to organ dysfunction needs an effective tool to predict the prognosis of shock septic. Early recognition and treatment of septic shock improved prognosis and reduced mortality, especially in pediatrics. This review aimed to identify the predictor of mortality in pediatric septic shock. Methods: We performed a literature review of the predictor of mortality in pediatric septic shock conducted between 2015 and 2020 in ProQuest, Google Scholar, PubMed, and Science Direct. We used keywords (predictor or predictive) and (septic shock or septic), and (prognostic or prognosis) and (pediatric or children). The study selection was using the Preferred Reporting Items for Systematic Review and Meta-Analysis PRISMA framework. Results: 944 articles identified in ProQuest, 720 articles in Science Direct, 339 articles in Google Scholar, and 67 in Pubmed. Equally, the total articles were 2,070 articles, and there were 414 duplicates. After review of the complete texts was performed for 35 potential studies. In the full-text review, we excluded review articles (n = 3), different populations (n=8), and of poor quality (n = 20). Eventually, four papers were reviewed in this study. We found PELOD, PELOD-2, PIM, PIM 2, PIM 3, PMODS, PRISM, PRISM-III, PRISM-IV, and pSOFA as a predictor of sepsis in pediatrics. Conclusion: In conclusion, pSOFA is a more accurate screening result for estimating the risk of death by being 10 times more sensitive and specific. However, adding biomarkers to pSOFA will improve the accuracy of the predictor prognosis of pediatric sepsis.
A debris disc under the influence of a wide planetary-mass companion: the system of HD 106906

The 13 Myr old star HD 106906 is orbited by a debris disk of at least 0:067 MMoon with an inner and outer radius of 20 AU and 120 AU, respectively, and by a planet at a distance of 650 AU. We use this curious combination of a close low-mass disk and a wide planet to motivate our simulations of this system. We study the parameter space of the initial conditions to quantify the mass loss from the debris disk and its lifetime under the inuence of the planet. We nd that when the planet orbits closer to the star than about 50 AU and with low inclination relative to the disk (less than about 10 ), more disk material is perturbed outside than inside the region constrained by observations on timescales shorter than 1 Myr. Considering the age of the system, such a short lifetime of the disk is incompatible with the timescale for planet{planet scattering which is one of the scenarios suggested to explain the wide separation of the planet. For some congurations when the planet orbit is inclined with respect to the disk, the latter will start to wobble. We argue that this wobbling is caused by a mechanism similar to the Kozai{Lidov oscillations. We also observe various resonant structures (such as rings and spiral arms) induced in the disk by the planet.
Azimuthal velocity profiles in Rayleigh-stable Taylor–Couette flow and implied axial angular momentum transport

We present azimuthal velocity profiles measured in a Taylor–Couette apparatus, which has been used as a model of stellar and planetary accretion disks. The apparatus has a cylinder radius ratio of ${\it\eta}=0.716$ , an aspect ratio of ${\it\Gamma}=11.74$ , and the plates closing the cylinders in the axial direction are attached to the outer cylinder. We investigate angular momentum transport and Ekman pumping in the Rayleigh-stable regime. This regime is linearly stable and is characterized by radially increasing specific angular momentum. We present several Rayleigh-stable profiles for shear Reynolds numbers $\mathit{Re}_{S}\sim O(10^{5})$ , for both ${\it\Omega}_{i}>{\it\Omega}_{o}>0$ (quasi-Keplerian regime) and ${\it\Omega}_{o}>{\it\Omega}_{i}>0$ (sub-rotating regime), where ${\it\Omega}_{i,o}$ is the inner/outer cylinder rotation rate. None of the velocity profiles match the non-vortical laminar Taylor–Couette profile. The deviation from that profile increases as solid-body rotation is approached at fixed $\mathit{Re}_{S}$ . Flow super-rotation, an angular velocity greater than those of both cylinders, is observed in the sub-rotating regime. The velocity profiles give lower bounds for the torques required to rotate the inner cylinder that are larger than the torques for the case of laminar Taylor–Couette flow. The quasi-Keplerian profiles are composed of a well-mixed inner region, having approximately constant angular momentum, connected to an outer region in solid-body rotation with the outer cylinder and attached axial boundaries. These regions suggest that the angular momentum is transported axially to the axial boundaries. Therefore, Taylor–Couette flow with closing plates attached to the outer cylinder is an imperfect model for accretion disk flows, especially with regard to their stability.
Variable turbulent convection as the cause of the Blazhko effect – testing the Stothers model

The amplitude and phase modulation observed in a significant fraction of the RR Lyrae variables - the Blazhko effect - represents a longstanding enigma in stellar pulsation theory. No satisfactory explanation for the Blazhko effect has been proposed so far. In this paper we focus on the Stothers idea, in which modulation is caused by changes in the structure of the outer convective zone, caused by a quasi-periodically changing magnetic field. However, up to this date no quantitative estimates were made to investigate whether such a mechanism can be operational and whether it is capable of reproducing the light variation we observe in Blazhko variables. We address the latter problem. We use a simplified model, in which the variation of turbulent convection is introduced into the non-linear hydrodynamic models in an ad hoc way, neglecting interaction with the magnetic field. We study the light-curve variation through the modulation cycle and properties of the resulting frequency spectra. Our results are compared with Kepler observations of RR Lyr. We find that reproducing the light-curve variation, as is observed in RR Lyr, requires a huge modulation of the mixing length, of the order of ±50 per cent, on a relatively short time-scale of less than 40 d. Even then, we are not able to reproduce all the observed relations between modulation components present in the frequency spectrum and the relations between Fourier parameters describing the shape of the instantaneous light curves.
On the role of shear in cosmological averaging

Using the spherically symmetric inhomogeneous Lemaȋtre-Tolman-Bondi dust solution, we study how the shear and the backreaction depend on the sharpness of the spatial transition between voids and walls and on the size of the voids. The voids considered here are regions with matter density Ω0 ≃ 0 and expansion rate H0t0 ≃ 1, while the walls are regions with matter density Ω0 ≃ 1 and expansion rate H0t0 ≃ 2/3. The results indicate that both the volume-average shear and the variance of the expansion rate grow proportional to the sharpness of the transition and diverge in the limit of a step function, but, for realistic-sized voids, are virtually independent of the size of the void. However, the backreaction, given by the difference of the variance and the shear, has a finite value in the step-function limit. By comparing the exact result for the backreaction to the case where the shear is neglected by treating the voids and walls as separate Friedmann-Robertson-Walker models, we find that the shear suppresses the backreaction by a factor of (r0/t0)2, the squared ratio of the void size to the horizon size. This exemplifies the importance of using the exact solution for the interface between the regions of different expansion rates and densities. The suppression is justified to hold also for a network of compensated voids, but may not hold if the universe is dominated by uncompensated voids.
Quench dynamics and relaxation in isolated integrable quantum spin chains

We review the dynamics after quantum quenches in integrable quantum spin chains. We give a pedagogical introduction to relaxation in isolated quantum systems, and discuss the description of the steady state by (generalized) Gibbs ensembles. We then turn to general features in the time evolution of local observables after the quench, using a simple model of free fermions as an example. In the second part we present an overview of recent progress in describing quench dynamics in two key paradigms for quantum integrable models, the transverse field Ising chain and the anisotropic spin-1/2 Heisenberg chain.
THE RADIO–2 mm SPECTRAL INDEX OF THE CRAB NEBULA MEASURED WITH GISMO

We present results of 2 mm observations of the Crab Nebula, obtained using the Goddard-IRAM Superconducting 2 Millimeter Observer (GISMO) bolometer camera on the IRAM 30 m telescope. Additional 3.3 mm observations with the MUSTANG bolometer array on the Green Bank Telescope are also presented. The integrated 2 mm flux density of the Crab Nebula provides no evidence for the emergence of a second synchrotron component that has been proposed. It is consistent with the radio power-law spectrum, extrapolated up to a break frequency of log (νb[GHz]) = 2.84 ± 0.29 or νb = 695+651− 336 GHz. The Crab Nebula is well resolved by the ∼16. ″7 beam (FWHM) of GISMO. Comparison to radio data at comparable spatial resolution enables us to confirm significant spatial variation of the spectral index between 21 cm and 2 mm. The main effect is a spectral flattening in the inner region of the Crab Nebula, correlated with the toroidal structure at the center of the nebula that is prominent in the near-IR through X-ray regime.
Global contrail coverage simulated by CAM5 with the inventory of 2006 global aircraft emissions

This paper documents the incorporation of an inventory of the AEDT (Aviation Environmental Design Tool) global commercial aircraft emissions for the year of 2006 into the National Center for Atmospheric Research Community Earth System Model (CESM) version 1. The original dataset reports aircraft emission mass of ten species on an hourly basis which is converted to monthly emission mixing ratio tendencies as the released version of the dataset. We also describe how the released aircraft emission dataset is incorporated into CESM. A contrail parameterization is implemented in the CESM in which it is assumed that persistent contrails initially form when aircraft water vapor emissions experience a favorable atmospheric environment. Both aircraft emissions and ambient humidity are attributed to the formation of contrails. The ice water content of contrails is assumed to follow an empirical function of atmospheric temperature which determines the cloud fraction associated with contrails. Our modeling study indicates that the simulated global contrail coverage is sensitive to the vertical resolution of the GCMs in the upper troposphere and lower stratosphere because of model assumptions about the vertical overlap structure of clouds. Furthermore, the extent of global contrail coverage simulated by CESM exhibits a seasonal cycle which is in broad agreement with observations.