Miracle-dz/UniFAR-FTUs huggingface dataset:
Influence of Supraglottal Geometry and Modeling Choices on the Flow-Induced Vibration of a Computational Vocal Fold Model

Influence of Supraglottal Geometry and Modeling Choices on the Flow-Induced Vibration of a Computational Vocal Fold Model Timothy E Shurtz Department of Mechanical Engineering, BYU Master of Science Computational models of the flow-induced vibrations of the vocal folds are powerful tools that can be used in conjunction with physical experiments to better understand voice production. This thesis research has been performed to contribute to the understanding of vocal fold dynamics as well as several aspects of computational modeling of the vocal folds. In particular, the effects of supraglottal geometry have been analyzed using a computational model of the vocal folds and laryngeal airway. In addition, three important computational modeling parameters (contact line location, Poisson's ratio, and symmetry assumptions) have been systematically varied to determine their influence on model output. Variations in model response were quantified by comparing glottal width, frequency, flow rate, open quotient, pressures, and wave velocity measures. In addition, the glottal jet was qualitatively analyzed. It was found that for various supraglottal geometries (either symmetrically or asymmetrically positioned), there was little asymmetry of the vocal fold motion despite significant asymmetry in the glottal jet. In addition, the vocal fold motion was most symmetric when consistent jet deflection was present (even if asymmetric). Inconsistent deflection of the glottal jet led to slightly larger asymmetries in vocal fold motion. The contact line location was found to have minimal impact on glottal width, frequency, and flow rate. The largest influence of the contact line location was seen in predicted velocity fields during the closed phase and in the pressure profiles along the vocal fold surfaces. Variations in Poisson's ratio strongly affected vocal fold motion, with lower Poisson's ratios resulting in larger amplitudes. The model did not vibrate when a Poisson's ratio of 0.49999 was used. The response of a full model (with two vocal folds) was shown to vary slightly from that of a half model (one vocal fold and a symmetry boundary condition), the greatest difference being in the deflection and dissipation of the glottal jet. It was concluded that for many scenarios the half model will be sufficient for modeling vocal fold motion; however, a full model is suggested for studies of material asymmetry or glottal jet dynamics. Application of these results to computational models of the vocal folds will lead to improved modeling and understanding of vocal fold dynamics.
Analytical approach for treating unitary quantum systems with initial mixed states

The mixed states are important in quantum optics since they frequently appear in the decoherence problems. When one of the components of the system is prepared in the mixed state and the evolution operator of this system is not available, one cannot deduce the density matrix. We present analytical approach to accurately solve this problem. The approach can be applied on the condition that the Schr\"odinger's equation of the system is solvable with any arbitrary initial state. In deriving the solution we exploit the fact that any mixed state can be expressed in terms of a phase state. The approach is illustrated by deriving the density matrix of a single-mode heat environment interacting asymmetrically with two qubits. Our results are in good agreement with the available results in the literature. This approach opens new perspectives for treating complicated systems and may impact other applications in the quantum theory.
Structure of Growing Networks: Exact Solution of the Barabasi--Albert's Model

We generalize the Barab´asi–Albert’s model of growing networks accounting for initial properties of sites and ﬁnd exactly the distribution of connectivities of the network P ( q ) and the averaged connectivity q ( s,t ) of a site s in the instant t (one site is added per unit of time). At long times P ( q ) ∼ q − γ at q → ∞ and q ( s, t ) ∼ ( s/t ) − β at s/t → 0, where the exponent γ varies from 2 to ∞ depending on the initial attractiveness of sites. We show that the relation β ( γ − 1) = 1 between the exponents is universal.
Stochastic 3d geometric models for classification, deformation, and estimation

In the thesis two new 3D stochastic shape models are proposed: (1) a model for the estimation and classification of 3D axially symmetric shapes, and (2) a model for the deformation of 3D free-form shapes. In (1), a system is described for the purpose of automatically estimating mathematical models for archaeological vessels given 3D measurements of their fragments commonly called sherds where it is assumed that the vessel is symmetric about a central axis. The unique approach integrates solutions to 4 different problems: (i) an algorithm for accurately estimating the surface geometry of individual sherds, (ii) an algorithm for accurately aligning assemblies of sherds, called configurations , (iii) a Bayesian performance measure for sherd configurations, and (iv) a performance-driven search algorithm. Estimation of the unknown geometry of the object is implemented as maximum likelihood estimation (MLE) where we seek to find the axially symmetric geometry which best explains the measured fragment data. For a configuration consisting of N sherds, this requires simultaneous estimation of N − 1 3D sherd alignment transformations, the matched sherd boundary curves, and the global shape of the axially symmetric surface. Configurations are constructed using a Bayesian performance measure which is the log of the probability of the computed configuration. The system merges sherds from a set of pairwise matches to generate larger sherd configurations and merges are done along contours of constant probability starting at the most probable merge. In (2), a new stochastic surface model for deformable 3D surfaces is proposed and its application to totally unconstrained 3D free-form surface sculpting is presented. A 3D surface is a sample of a Markov Random Field (MRF) defined on the vertices of a 3D mesh where MRF sites coincide with mesh vertices and MRF cliques consist of subsets of sites. Each site has 3D coordinates (x,y,z) as random variables and is a random vector in one or more clique potentials which are functions defined on the sites within a clique and describe stochastic dependencies among sites. Data, which is used to deform the surface, can consist of, but is not limited to, an unorganized set of 3D points and is modeled by a conditional probability distribution given the 3D surface. A deformed surface is a MAP (Maximum A-posteriori Probability) estimate and is the deformed surface for which the joint distribution of the MRF surface model and the data is maximum. Included in the development is the introduction of a virtual sculpting system which integrates new data models, new anisotropic clique potentials, and cliques which involve sites that are spatially far apart.
Selected Topics In Shock Wave Physics And Equation Of State Modeling

Fundamental results for plane shock waves Hugoniot relations for shock waves with curved surfaces stability of shock waves rarefaction waves method of characteristics Hugoniots for porous materials Hugoniot measurement methods sound speed measurement techniques release isentrope measurement techniques measurement of the Gruneisen coefficient equation of state modelling calculation of thermodynamic, Slater and Dugdale-McDonald Gruneisen parameters for analytic equations of state calculation of the principal Hugoniot for an analytic equation of state. Appendices: solution of the cubic with real coefficients multi-branched equation of state for lithium useful computer routines for plane shock waves.
High speed switching in magnetic recording thin-film heads

There has always been an increasing demand for high density data storage. However, the increased areal storage densities of hard disk drives require a level of miniturisation of the recording heads where the micromagnetic details and switching mechanisms can no longer be ignored. Furthermore, theoretical and numerical studies on thin-film recording heads tend to separate the micromagnetics from the electromagnetic aspects of the head during switching and hence ignore the lossy nature of head materials. This project was aimed to develop a numerical simulation approach that simultaneously incorporates the fundamental micromagnetic and electromagnetic details of magnetic materials to study the fast switching process in soft magnetic materials in general, and in thin-film inductive writers in particular. The project also was aimed at establishing an impedance measurement system to characterise losses in magnetic recording heads, and to allow comparison with the simulations. This project successfully met all its original objectives. A numerical technique to simulate the dynamic behaviour of magnetic materials and devices has been developed, and applied to study the switching process in thin-film recording heads. Two-dimensional simulations of complete commercial head structures including the coils and pole regions were carried out and parameters such as gap field rise times, gap field distributions, and core inductances, which are important for head designers, were predicted. Moreover, the role of eddy currents delaying the magnetisation switching was elucidated. Furthermore, it was found that the gradient of the recording fields were sharper near the conrner regions of the poles when considering magnetic details. A high precision, high bandwidth impedance measurement system was established to characterise losses in magnetic heads. Fittings of measured core inductances to a proposed equivalent circuit model of the core’s relaxation processes revealed the switching times of heads (of the order 0.1 to 1.0ns).
Hubble Space Telescope/Faint Object Spectrograph Observations of M87:Lyα Emission from the Active Galactic Nucleus

The Faint Object Spectrograph on the Hubble Space Telescope was used to obtain spectra of the central region of M87. These spectra cover the wavelength range 1140-1606 Å and have a resolution of ~1 Å. The nuclear continuum is clearly visible in the spectra. The only strong line that is observed is Lyα, which has a velocity width of about 3000 km s-1 (higher than the width of any line previously observed in the M87 nucleus). There is also a marginal detection of C IV λ1549. The ratio of Lyα to C IV in the nuclear spectrum is at least a factor of 2 higher than in a spectrum taken at a position on the disk ~0. ″6 away from the nucleus by Dopita et al. This enhancement of Lyα at the nucleus could point to significant differences in the properties of the emitting gas and/or the excitation mechanism between the outer and inner disk regions. The strength of the observed Lyα places limits on the properties of the absorbing gas present within M87. For instance, if the hydrogen column at the systemic velocity of M87 is greater than about 1018 cm-2, then it can cover only a small fraction of the line-emitting region. Spectra separated by 5 days show a 60% difference in the Lyα flux, but the same continuum level. This could either be due to a displacement between the aperture positions for the two sets of observations, or it could be due to intrinsic variability of the source. The current observations do not strongly favor either of these alternatives. The observations do show, however, that the Lyα line is a useful tracer of kinematics in the M87 nucleus.
Fluid rings and droplet arrays via rim streaming

Tip-streaming generates micronand submicronsized droplets when a thin thread pulled from the pointy end of a drop disintegrates. Here, we report streaming from the equator of a drop placed in a uniform electric field. The instability generates concentric fluid rings encircling the drop, which break up to form an array of microdroplets in the equatorial plane. We show that the streaming results from an interfacial instability at the stagnation line of the electrohydrodynamic flow, which creates a sharp rim. The flow draws from the rim a thin sheet which destabilizes and sheds fluid cylinders. This streaming phenomenon provides a new route for generating monodisperse microemulsions.
VESTIGE OF THE STAR CLUSTER BURST IN M51

We present a study of the star cluster formation in M51 based on the image data taken with Advanced Camera for Surveys (ACS) and Wide Field Planetary Camera 2 (WFPC2) of Hubble Space Telescope (HST). We have derived the star cluster formation rate using the ages and masses of about 2000 star clusters estimated by comparing photometric data (F336W, F435W, F555W, and F814W) with theoretical population synthesis models. The star cluster formation rate increased significantly during the period of 100–250 Myr ago. This period roughly coincides with the epoch of dynamical encounters of two galaxies, NGC 5194 and NGC 5195, expected by theoretical models. The age distribution of the star clusters also shows two peaks at about 100 Myr and 250 Myr ago. The star cluster mass ranges from 103 to 106 M☉ and the mass function can be represented by a power law with an index ranging from α = −2.23 ± 0.34 for t < 10 Myr to α = −1.37 ± 0.11 for t>100 Myr. The mass function of star clusters older than 10 Myr also appears to display the steepest distribution with α ≈ −1.50 at around 200 Myr ago, near the expected epoch of the galaxy interaction. We also confirm the correlations of cluster size increasing with cluster mass (with a best-fit slope of 0.16 ± 0.02), and with cluster age (0.14 ± 0.03).
An Unorthodox Parametric Measure of Information and Corresponding Measure of Intutionistic Fuzzy Information

A new parametric function is proposed for the probability distribution and its properties are studied. In this paper the given functions is twice differentiable and is used to obtain the related measure of directed divergence, measure of intutionistic fuzzy entropy, measure of intutionistic fuzzy directed divergence. We also investigate the monotonic character of the proposed function.
Modelling the supernova-driven ISM in different environments

We use hydrodynamical simulations in a $(256\;{\rm pc})^3$ periodic box to model the impact of supernova (SN) explosions on the multi-phase interstellar medium (ISM) for initial densities $n = 0.5-30$ cm$^{-3}$ and SN rates $1-720$ Myr$^{-1}$. We include radiative cooling, diffuse heating, and the formation of molecular gas using a chemical network. The SNe explode either at random positions, at density peaks, or both. We further present a model combining thermal energy for resolved and momentum input for unresolved SNe. Random driving at high SN rates results in hot gas ($T\gtrsim 10^6$ K) filling $> 90$% of the volume. This gas reaches high pressures ($10^4 50$%), residing in small, dense clumps. Such a model might resemble the dense ISM in high-redshift galaxies. Peak driving results in huge radiative losses, producing a filamentary ISM with virtually no hot gas, and a small molecular hydrogen mass fraction ($\ll 1$%). Varying the ratio of peak to random SNe yields ISM properties in between the two extremes, with a sharp transition for equal contributions. The velocity dispersion in HI remains $\lesssim 10$ km s$^{-1}$ in all cases. For peak driving the velocity dispersion in H$_\alpha$ can be as high as $70$ km s$^{-1}$ due to the contribution from young, embedded SN remnants.
GDH Integral on the Proton from Asymmetries

Inclusive double spin electron asymmetries have been measured by scattering polarized electrons off the solid polarized {sup 15}NH{sub 3} target in Hall B of Jefferson Lab in 2000-2001. The virtual photon asymmetry A{sub 1} (x), the longitudinal spin structure function, g{sub 1} (x, Q{sup 2}), and the first moment, {Gamma}{sub 1}{sup p}, have been evaluated for a kinematic range of 0.05 {ge} Q{sup 2} {ge} 4.5 GeV{sup 2}. The extracted results complement the existing data in the resonance region, extending it to lower and higher Q{sup 2} regions. The results are important in the study of Q{sup 2} evolution of nucleon structure from the hadronic to partonic degrees of freedom.
The Interstellar Medium around the Supernova Remnant G320.4−1.2

Using the Australia Telescope Compact Array, we have carried out a survey of the H I emission in the direction of the barrel-shaped supernova remnant (SNR) G320.4-1.2 (MSH 15-52) and its associated young pulsar B1509-58. The angular resolution of the data is 4. ′0 × 2. ′7, and the rms noise is of order 30 mJy beam-1 (∼0.5 K). The H I observations indicate that the north-northwest radio limb has encountered a dense H I filament (density ∼12 cm-3) at the same LSR velocity as that of the SNR (VLSR ∼ -68 km s-1). This H I concentration would be responsible for the flattened shape of the northwestern lobe of G320.4-1.2 and for the formation of the radio-optical–X-ray nebula RCW 89. The emission associated with the bright knots in the interior of RCW 89 can be explained as arising from the interaction between the collimated relativistic outflow from the pulsar and the denser part of this H I filament (density ∼15 cm-3). The south-southeastern half of the SNR, on the other hand, seems to have rapidly expanded across a lower density environment (density ∼0.4 cm-3). The H I data also reveal an unusual H I feature aligned with a collimated outflow generated by the pulsar, suggestive of association with the SNR. The anomalous kinematical velocity of this feature (VLSR ∼ 15 km s-1), however, is difficult to explain.
BROAD N2H+ EMISSION TOWARD THE PROTOSTELLAR SHOCK L1157-B1

We present the first detection of N2H+ toward a low-mass protostellar outflow, namely, the L1157-B1 shock, at ∼0.1 pc from the protostellar cocoon. The detection was obtained with the IRAM 30 m antenna. We observed emission at 93 GHz due to the J = 1–0 hyperfine lines. Analysis of this emission coupled with HIFI CHESS multiline CO observations leads to the conclusion that the observed N2H+(1–0) line originated from the dense (⩾105 cm−3) gas associated with the large (20″–25″) cavities opened by the protostellar wind. We find an N2H+ column density of a few 1012 cm−2 corresponding to an abundance of (2–8) × 10−9. The N2H+ abundance can be matched by a model of quiescent gas evolved for more than 104 yr, i.e., for more than the shock kinematical age (≃2000 yr). Modeling of C-shocks confirms that the abundance of N2H+ is not increased by the passage of the shock. In summary, N2H+ is a fossil record of the pre-shock gas, formed when the density of the gas was around 104 cm−3, and then further compressed and accelerated by the shock.
TESTING NONSTANDARD COSMOLOGICAL MODELS WITH SNLS3 SUPERNOVA DATA AND OTHER COSMOLOGICAL PROBES

We investigate the implications for some nonstandard cosmological models using data from the first three years of the Supernova Legacy Survey (SNLS3), assuming a spatially flat universe. A comparison between the constraints from the SNLS3 and those from other SN Ia samples, such as the ESSENCE, Union2, SDSS-II, and Constitution samples, is given and the effects of different light-curve fitters are considered. We find that analyzing SNe Ia with SALT2 or SALT or SiFTO can give consistent results and the tensions between different data sets and different light-curve fitters are obvious for fewer-free-parameters models. At the same time, we also study the constraints from SNLS3 along with data from the cosmic microwave background and the baryonic acoustic oscillations (CMB/BAO), and the latest Hubble parameter versus redshift (H(z)). Using model selection criteria such as χ2/dof, goodness of fit, Akaike information criterion, and Bayesian information criterion, we find that, among all the cosmological models considered here (ΛCDM, constant w, varying w, Dvali–Gabadadze–Porrati (DGP), modified polytropic Cardassian, and the generalized Chaplygin gas), the flat DGP is favored by SNLS3 alone. However, when additional CMB/BAO or H(z) constraints are included, this is no longer the case, and the flat ΛCDM becomes preferred.
Monitoring electrostatically-induced deflection, strain and doping in suspended graphene using Raman spectroscopy

Electrostatic gating offers elegant ways to simultaneously strain and dope atomically thin membranes. Here, we report on a detailed in situ Raman scattering study on graphene, suspended over a Si/SiO2 substrate. In such a layered structure, the intensity of the Raman G- and 2D-mode features of graphene are strongly modulated by optical interference effects and allow an accurate determination of the electrostatically-induced membrane deflection, up to irreversible collapse. The membrane deflection is successfully described by an electromechanical model, which we also use to provide useful guidelines for device engineering. In addition, electrostatically-induced tensile strain is determined by examining the softening of the Raman features. Due to a small residual charge inhomogeneity, we find that non-adiabatic anomalous phonon softening is negligible compared to strain-induced phonon softening. These results open perspectives for innovative Raman scattering-based readout schemes in two-dimensional nanoresonators.
Revision of the energy calibration of the Yakutsk extensive air shower array

Responses of surface and underground scintillation detectors of Yakutsk array are calculated for showers initiated by primary particles with energy E0>=1.0E17 eV within the frameworks of QGSJet01 QGSIIJet-II-04, SIBYLL-2.1 and EPOS-LHC hadron interaction models. A new estimation of E0 is obtained with the use of various methods. The resulting energy is lower compared to the obtained with earlier method by factor ~1.33.
Piezoelectric properties of (Bi1/2Na1/2)TiO3 based ceramics

Abstract In this paper, piezoelectric properties of (Bi1/2Na1/2)1–x (Sr1/2Ca1/2) x TiO3 system were studied from the viewpoint of lead-free piezoelectric materials. To improve electromechanical properties in this system, MnO was added to this system. In the composition of x = 0.13 which was close to morphotropic phase boundary (MPB), electromechanical properties such as kt and Qm were increasing with increase of the amount of MnO and took maximum value (kt ≊ 47%, Qm ≊ 367) at about 0.4 wt. % On the other hand, dielectric constant ϵ r was decreasing with it and took comparatively lower value (ϵ33/ϵ0 = 518).
Modeling of radiation-induced defect recovery in 3C-SiC under high field bias conditions

In this work, the implications of high field bias conditions in radiation-induced defect recovery in 3C-SiC crystals is studied. It is well known that transient heating effects (or thermal spikes) occur when energetic swift heavy ions (SHIs) deposit energy to the surrounding medium via ionization. Here, we explore the dynamics of this transient event under high background electric fields in 3C-SiC, which is what occurs when an ion strike coincides with field-sensitive volumes. In this study, we use the Ensemble Monte Carlo method to quantify how the energy deposition of the ionized regions change in response to high background electric fields. Subsequently, we study the relationship between the radiation-induced thermal spike and defect recovery using molecular dynamics simulations. We find that field strengths below the critical breakdown of wide bandgap devices are sufficient to exacerbate the localized heating, which subsequently enhances the defect recovery effect. This work is beneficial for 3C-SiC electronics and materials used in high radiation environments.