Intrinsic Shape Research Articles

Magneto-optical studies of kerosene based ferrofluid

Magnetic fluids are technologically important due to their tunable magnetic, electrical and optical properties. The magneto optical properties of ferrofluid have a major role for the development of optoelectronic devices. This paper represents the detailed analysis of kerosene based ferrofluid, their structure and magneto optical properties will be investigated. Iron oxide nanofluids are synthesised by a Co-precipitation method. The X-ray diffraction technique is used for structural characterization. The magneto optical property of the iron oxide nanofluid have been investigated by linear dichroism measurements. Individual magnetic particle’s intrinsic optical anisotropy or shape anisotropy create linear dichroism. The magnetic susceptibility of ferrofluid with different volume fractions is measured using Quincke’s method.

Accounting for shape factor effects in Ogden-Hill elastomeric foam model

Abstract A framework for the determination of shape-factor dependent parameters in the constitutive models of elastomeric foams, to account for the shape factor effect in quasi-static pressure-strain response of elastomeric foam isolators, is presented. The methodology is an empirical-based method which is applied to the Ogden-Hill foam model. There is no information or model in the literature to account for the shape factor effect on mechanical behaviour of elastomeric foams. Also, none of the existing models of elastomeric foam including Ogden-Hill model are able to predict accurately the pressure-strain response of vibrational isolation systems designed with elastomeric foam isolator pads/strips of different sizes or shape factors. The reason is that all the parameters in such models are a function of material intrinsic property alone which have constant values irrespective of the size of the pads/strips. Therefore, the aim of this study is to derive a set of empirical shape factor dependent parametric functions μ ( s ) and β ( s ) , and to apply them instead of constant parameters μ and β in Ogden-Hill model. This will enable the model to take the shape factor (s) of the pads/strips into account when predicting the pressure-strain response of an elastomeric foam-based system. The study involved testing of polyurethane (PU) pads/strip samples of different sizes and densities (160, 270 and 385 kg/m 3 ) at a displacement rate of 5 mm/min up to 30% compressive strain. Analysis of the measured data showed that the static stiffness of an elastomeric foam-based system increases under a constant compressive load when the shape factor of the pads/strips increases. This implies that the compression modulus of such systems should be a function of both intrinsic material property and shape factor. The test results show that μ ( s ) and β ( s ) are nonlinear functions of the shape factor. The predictions using the derived shape factor-dependent parameters in Ogden-Hill model show good agreement with the measured pressure-strain response of the tested pads/strips. They show that the accuracy of the predicted pressure at, for example, 15% strain is higher than 90% for most of the samples. • Shape factor independent parameters μ and β in Ogden-Hill model give large errors. • Errors minimised by use of shape factor dependent material parameters μ ( s ) and β ( s ) • Derivation of μ ( s ) and β ( s ) from compression stress-strain data of different samples. • Polyurethane pads of different shape factors and densities tested up to 30% strain. • Prediction errors of Ogden-Hill model using μ ( s ) and β ( s ) mostly less than 10%.

Mapping the X-Ray Corona Evolution of IRAS 13224-3809 with the Power Spectral Density

We develop the power spectral density (PSD) model to explain the nature of the X-ray variability in IRAS 13224–3809, including the full effects of the X-ray reverberation due to the lamppost source. We utilize 16 XMM-Newton observations individually as well as group them into three different luminosity bins: low, medium, and high. The soft (0.3–1 keV) and hard (1.2–5 keV) PSD spectra are extracted and simultaneously fitted with the model. We find that the corona height changes from h ∼ 3 r g during the lowest luminosity state to ∼25 r g during the highest luminosity state. This provides further evidence that the source height from the reverberation data is significantly larger than what is constrained by the spectral analysis. Furthermore, as the corona height increases, the energy spectrum tends to be softer while the observed fractional excess variance, F var, reduces. We find that the PSD normalization is strongly correlated with F var and moderately correlated with the PSD bending index. Therefore, the normalization is dependent on the accretion rate that controls the intrinsic shape of the PSD. While the intrinsic variability of the disk is manifested by the reverberation signals, the disk and corona may evolve independently. Our results suggest that, as the source height increases, the disk itself generates less overall variability power but more high-frequency variability resulting in the PSD spectrum that flattens out (i.e., the inner disk becomes more active). Using the luminosity-bin data, the hint of the Lorentzian component is seen, with the peak appearing at lower frequencies with increasing luminosity.

Redshift and stellar mass dependence of intrinsic shapes of disc-dominated galaxies from COSMOS observations below z = 1.0

ABSTRACT The high abundance of disc galaxies without a large central bulge challenges predictions of current hydrodynamic simulations of galaxy formation. We aim to shed light on the formation of these objects by studying the redshift and mass dependence of their intrinsic 3D shape distributions in the COSMOS galaxy survey below redshift z = 1.0. This distribution is inferred from the observed distribution of 2D shapes, using a reconstruction method which we test using hydrodynamic simulations. Our tests reveal a moderate bias for the inferred average disc circularity and relative thickness, but a large bias on the dispersion of these quantities. Applying the reconstruction method on COSMOS data, we find variations of the average disc circularity and relative thickness with redshift of around ∼1 per cent and ∼10 per cent, respectively, which is comparable to the error estimates on these quantities. The average relative disc thickness shows a significant mass dependence which can be accounted for by the scaling of disc radius with galaxy mass. We conclude that our data provides no evidence for a strong dependence of the average circularity and absolute thickness of disc-dominated galaxies on redshift and mass that is significant with respect to the statistical uncertainties in our analysis. These findings are expected in the absence of disruptive merging or feedback events that would affect galaxy shapes. They hence support a scenario where present-day discs form early ( z > 1.0) and subsequently undergo a tranquil evolution in isolation. However, more data and a better understanding of systematics are needed to reaffirm our results.

Cardanol-derived anhydride cross-linked epoxy thermosets with intrinsic anti-flammability, toughness and shape memory effect

With the increasing awareness of environmental protection, the development of high-performance bio-based epoxy resins has attracted more and more attention to reduce the dependence on the petroleum-based 4,4′-diaminodiphenylmethane (DDM). In this work, we synthesized two kinds of cardanol-based curing agents (Car-DCP-MAH and Car-DPC-MAH) as alternatives for petroleum-based DDM. The chemical structures of Car-DCP-MAH and Car-DPC-MAH were confirmed by 1H and 31P NMR. Compared with the traditional DGEBA/DDM thermoset, the cured DGEBA/Car-DCP-MAH and DGEBA/Car-DPC-MAH thermosets both displayed good intrinsic fire resistance in terms of higher LOI values (29% and 28%, respectively, versus 24.5%) and V-0 rating in the UL-94 test. Furthermore, the results of the cone calorimeter test showed a significant reduction in the peak heat release rate (PHRR) values of the cured DGEBA/Car-DCP-MAH and DGEBA/Car-DPC-MAH which were 42.3% and 47.7%. The flame retardancy of these two systems was mainly due to the great carbonization ability and the formation of the intact and compact char layer. Owning to the flexible long alkyl chain in the crosslinking network, the toughness of the cured DGEBA/Car-DCP-MAH and DGEBA/Car-DPC-MAH products was greatly improved with the higher elongation at break and impact strength. Additionally, the cured DGEBA/Car-DCP-MAH and DGEBA/Car-DPC-MAH thermosets both showed preferable shape memory properties with a high shape recovery efficiency of 98.6% and 96.3%. This study provides a novel strategy to achieve bio-based epoxy thermosets with intrinsic anti-flammability, toughness and shape memory effect.

NeuralTailor

The fields of SocialVR, performance capture, and virtual try-on are often faced with a need to faithfully reproduce real garments in the virtual world. One critical task is the disentanglement of the intrinsic garment shape from deformations due to fabric properties, physical forces, and contact with the body. We propose to use a garment sewing pattern, a realistic and compact garment descriptor, to facilitate the intrinsic garment shape estimation. Another major challenge is a high diversity of shapes and designs in the domain. The most common approach for Deep Learning on 3D garments is to build specialized models for individual garments or garment types. We argue that building a unified model for various garment designs has the benefit of generalization to novel garment types, hence covering a larger design domain than individual models would. We introduce NeuralTailor, a novel architecture based on point-level attention for set regression with variable cardinality, and apply it to the task of reconstructing 2D garment sewing patterns from the 3D point cloud garment models. Our experiments show that NeuralTailor successfully reconstructs sewing patterns and generalizes to garment types with pattern topologies unseen during training.

Formulation and Evaluation of Dry Powder Inhaler

Abstract: This review focuses on the dry powder inhaler (DPI) formulation and development process. Most DPI formulations consist of micronized drug blended with larger carrier particles, which enhance flow, reduce aggregation, and aid in dispersion. A combination of intrinsic physicochemical properties, particle size, shape, surface area, and morphology affects the forces of interaction and aerodynamic properties, which in turn determine fluidization, dispersion, delivery to the lungs, and deposition in the peripheral airways. When a DPI is actuated, the formulation is fluidized and enters the patient’s airways. Under the influence of inspiratory airflow, the drug particles separate from the carrier particles and are carried deep into the lungs, while the larger carrier particles impact on the oropharyngeal surfaces and are cleared. If the cohesive forces acting on the powder are too strong, the shear of the airflow may not be sufficient to separate the drug from the carrier particles, which results in low deposition efficiency. This review thus demonstrates that the successful delivery of dry powder aerosols to the lung requires careful consideration of the powder production process, formulation and inhaler device. The developments and improvements towards high dose powder pulmonary drug delivery are summarized and discussed here. It also throws light on the invention and improvement of novel inhaler devices as well as the further development of formulation principles and new powder engineering methods.

Monitoring observations of SMC X-1’s excursions (MOOSE)–I. Programme description and initial high state spectral results

ABSTRACT SMC X-1 has exhibited three superorbital period excursions since the onset of X-ray monitoring beginning with the Rossi X-ray Timing Explorer's launch in 1995. TheNeutron star Interior Composition Explorer has recently probed a fourth observed excursion beginning in 2021 with our programme monitoring observations of SMC X-1’s excursions (moose). These sensitive new moose data probe different superorbital periods and phases within them. Spectral fits to the high-state continuum during 2021 April to 2022 January show that the intrinsic spectral shapes are characterized by a soft (kT ∼ 0.19 keV) disc component and a hard (Γ ∼ 0.7) power-law tail. When the 2021–2022 NICER observations, taken during an excursion, are compared to 2016 XMM–Newton observations (outside of an excursion), we find little evidence for intrinsic spectral variability across the high states, but find evidence for a >3σ change in the absorption, although we caution that there may be calibration differences between the two instruments. Thus, over different lengths of superorbital periods, we see little evidence for intrinsic spectral changes in the high state. Upcoming studies of the pulse profiles may shed light on the mechanism behind the excursions.

The In Situ Origins of Dwarf Stellar Outskirts in FIRE-2

Extended, old, and round stellar halos appear to be ubiquitous around high-mass dwarf galaxies (108.5 < M ⋆/M ⊙ < 109.6) in the observed universe. However, it is unlikely that these dwarfs have undergone a sufficient number of minor mergers to form stellar halos that are composed of predominantly accreted stars. Here, we demonstrate that FIRE-2 (Feedback in Realistic Environments) cosmological zoom-in simulations are capable of producing dwarf galaxies with realistic structures, including both a thick disk and round stellar halo. Crucially, these stellar halos are formed in situ, largely via the outward migration of disk stars. However, there also exists a large population of “nondisky” dwarfs in FIRE-2 that lack a well-defined disk/halo and do not resemble the observed dwarf population. These nondisky dwarfs tend to be either more gas-poor or to have burstier recent star formation histories than the disky dwarfs, suggesting that star formation feedback may be preventing disk formation. Both classes of dwarfs underscore the power of a galaxy’s intrinsic shape—which is a direct quantification of the distribution of the galaxy’s stellar content—to interrogate the feedback implementation in simulated galaxies.

Intrinsic alignments of bulges and discs

ABSTRACT Galaxies exhibit coherent alignments with local structure in the Universe. This effect, called intrinsic alignments (IAs), is an important contributor to the systematic uncertainties for wide-field weak lensing surveys. On cosmological distance scales, intrinsic shape alignments have been observed in red galaxies, which are usually bulge-dominated; while blue galaxies, which are mostly disc-dominated, exhibit shape alignments consistent with a null detection. However, disc-dominated galaxies typically consist of two prominent structures: disc and bulge. Since the bulge component has similar properties as elliptical galaxies and is thought to have formed in a similar fashion, naturally one could ask whether the bulge components exhibit similar alignments as ellipticals? In this paper, we investigate how different components of galaxies exhibit IA in the TNG100-1 cosmological hydrodynamical simulation, as well as the dependence of IA on the fraction of stars in rotation-dominated structures at $z$ = 0. The measurements were controlled for mass differences between the samples. We find that the bulges exhibit significantly higher IA signals, with a non-linear alignment model amplitude of $A_I = 2.98^{+0.36}_{-0.37}$ compared to the amplitude for the galaxies as a whole (both components), $A_I = 1.13^{+0.37}_{-0.35}$. The results for bulges are statistically consistent with those for elliptical galaxies, which have $A_I = 3.47^{+0.57}_{-0.57}$. These results highlight the importance of studying galaxy dynamics in order to understand galaxy alignments and their cosmological implications.

3D intrinsic shapes of quiescent galaxies in observations and simulations

ABSTRACT We study the intrinsic 3D shapes of quiescent galaxies over the last half of cosmic history based on their axial ratio distribution. To this end, we construct a sample of unprecedented size, exploiting multiwavelength u-to-Ks photometry from the deep wide-area surveys KiDS+VIKING paired with high-quality i-band imaging from HSC-SSP. The dependences of the shapes on mass, redshift, photometric bulge prominence and environment are considered. For comparison, the intrinsic shapes of quenched galaxies in the IllustrisTNG simulations are analysed and contrasted with their formation history. We find that over the full 0 &amp;lt; z &amp;lt; 0.9 range, and in both simulations and observations, spheroidal 3D shapes become more abundant at $M_* \gt 10^{11}\, \mathrm{M}_{\odot }$, with the effect being most pronounced at lower redshifts. In TNG, the most massive galaxies feature the highest ex situ stellar mass fractions, pointing to violent relaxation via mergers as the mechanism responsible for their 3D shape transformation. Larger differences between observed and simulated shapes are found at low to intermediate masses. At any mass, the most spheroidal quiescent galaxies in TNG feature the highest bulge mass fractions, and, conversely, observed quiescent galaxies with the highest bulge-to-total ratios are found to be intrinsically the roundest. Finally, we detect an environmental influence on galaxy shape, at least at the highest masses, such that at fixed mass and redshift, quiescent galaxies tend to be rounder in denser environments.

High-throughput finite-element design of dielectric composites for high-frequency copper clad laminates

Dielectric substrates with low dielectric constant and good thermal stability are highly desired for high-frequency and high-speed signal transmission. It is however challenging to rationally design the demand-satisfied polymer-based composites due to the inadequate understanding of the contradictory effect of inorganic fillers on modulating dielectric-thermal-mechanical properties. In this work, taking Polytetrafluoroethylene (PTFE)-SiO2 composite as the example, we perform high-throughput finite-element calculations to systematically study the filler effects on the dielectric constant of composites εrcomposite and the coefficient of thermal expansion of composites (CTE-c). A series of influencing factors including intrinsic property, volume fraction, shape, distribution, and orientation of fillers have been considered in our models to establish the structure-property mapping of dielectric composites. It is found that CTE-c is more sensitive to the filler structure of PTFE-SiO2 composites than εrcomposite. Finally, guided by the calculation results, a skeleton structure is proposed to realize the performance targets of εrcomposite< 2.3 and CTE-c < 60 ppm/K with lower SiO2 filler content. This work provides a universal data-driven strategy for the rational design of dielectric composites with multi-objective requirements, and it is expected to spark more experimental efforts to design novel dielectric composites for high-quality signal transmission.

Intrinsic traits, social context, and local environment shape home range size and fidelity of sleepy lizards

AbstractHome ranges (HRs), the regions within which animals interact with their environment, constitute a fundamental aspect of their ecology. HR sizes and locations commonly reflect costs and benefits associated with diverse social, biotic, and abiotic factors. Less is known, however, about how these factors affect intraspecific variation in HR size or fidelity (the individual's tendency to maintain the same HR location over time) or whether variation in these features emerge from consistent differences among individuals or among the sites they occupy. To address this knowledge gap, we used an extensive GPS‐tracking data set of a long‐lived lizard, the sleepy lizard (Tiliqua rugosa), which included repeated observations of multiple individuals across years. We tested how three categories of predictors—(1) lizard characteristics (sex, aggressiveness, and parasitic tick counts), (2) environmental characteristics (precipitation, food, and refuge quality), and (3) social conditions (conspecific overlap and number of neighbors)—affected HR size and fidelity. We found that individuals differed consistently in the size and fidelity of annual HRs (with a repeatability of 0.58 and 0.33, respectively), and that all three categories of predictors affected both HR size and fidelity. For example, HRs were smaller in areas with more food, and males had larger HRs than females. In addition, more aggressive lizards tended to have larger HRs. Conspecific overlap and number of individuals that a lizard interacted with (social network degree) had an interactive effect on HR size where individuals whose HRs overlapped more with neighbors had larger HRs, and this effect was particularly strong for individuals that interacted with more neighbors. HR fidelity declined over time (HR locations drifted from year to year), but individuals differed consistently in this rate of drift. The fact that HR size was consistent despite drifting locations suggests that lizard HRs reflect individual traits (e.g., habitat choice criteria that differ among individuals), rather than simple heterogeneity among sites. Overall, these findings demonstrate (1) both strong, long‐term, within‐individual consistency and between‐individual differences in space use and (2) combined effects of individual traits, social conditions, and environmental characteristics on animal HRs, with implications for diverse ecological processes.

How Followers’ Perception of Insider Status Influences the Relationship Between Servant Leadership and Work Attitude?

Servant leadership starts with an individual whose main interests are to serve, inspire and lead followers. Thus, the servant leader is an individual who is always pursuing and looking for better ways to achieve shared goals with fellow workers. The current study investigates the influencing mechanism of servant leadership on job satisfaction based on the social identity theory. Specifically, the purpose of this study is to develop a model of perceived insider status that mediates the relationships between servant leadership and employee job satisfaction. Data were collected from matched 90 leaders and 285 followers from the service industry in Taiwan. To avoid common method variance issue, we collected data across three-time points from two different sources. The statistical analyses included descriptive analysis, correlational approach, confirmatory factor analysis, and multi-level analyses. Using the bootstrapping method, the indirect effects of servant leadership on job satisfaction via perceived insider status were found to be significant. This study underscores the importance of encouraging leaders to engage in servant leader behaviors, thereby enhancing followers’ perception as insiders and improving followers' job satisfaction. Since servant leaders focus on employee-oriented tactics, it is essential to train leaders to enhance followers’ intrinsic motivation and shape their perceptions of belongingness and effectiveness.

Ultra-wide-temperature-range superelasticity and intrinsic two-way shape memory effect in Co–Ni–Ga microwires

We demonstrate perfect superelasticity and inherent two-way shape memory effect in Co49Ni21Ga30 microwires fabricated by a Taylor–Ulitovsky method. With the formation of an almost complete [001]A-oriented single crystal along the axis of the wire, the as-drawn microwire displays great superelastic behaviors with a large reversible tensile strain of &amp;gt;8% over an ultra-wide temperature window of 550 K (223–773 K). Simultaneously, an excellent intrinsic two-way shape memory effect with a considerably large strain output (∼6.3%) was also obtained in this Co49Ni21Ga30 microwire. After mechanical training, the two-way shape memory strain can reach up to 6.8% at a low operating temperature. With the combination of above extraordinary functional properties and the low cost of fabrication, the Co49Ni21Ga30 microwire holds a significant potential for applications in miniature sensing and self-actuating devices in the future.

The MASSIVE Survey. XVII. A Triaxial Orbit-based Determination of the Black Hole Mass and Intrinsic Shape of Elliptical Galaxy NGC 2693

Abstract We present a stellar dynamical mass measurement of a newly detected supermassive black hole (SMBH) at the center of the fast-rotating, massive elliptical galaxy NGC 2693 as part of the MASSIVE survey. We combine high signal-to-noise ratio integral field spectroscopy (IFS) from the Gemini Multi-Object Spectrograph with wide-field data from the Mitchell Spectrograph at McDonald Observatory to extract and model stellar kinematics of NGC 2693 from the central ∼150 pc out to ∼2.5 effective radii. Observations from Hubble Space Telescope WFC3 are used to determine the stellar light distribution. We perform fully triaxial Schwarzschild orbit modeling using the latest TriOS code and a Bayesian search in 6D galaxy model parameter space to determine NGC 2693's SMBH mass (M BH), stellar mass-to-light ratio, dark matter content, and intrinsic shape. We find M BH = 1.7 ± 0.4 × 10 9 M ⊙ and a triaxial intrinsic shape with axis ratios p = b/a = 0.902 ± 0.009 and q = c / a = 0.721 − 0.010 + 0.011 , triaxiality parameter T = 0.39 ± 0.04. In comparison, the best-fit orbit model in the axisymmetric limit and (cylindrical) Jeans anisotropic model of NGC 2693 prefer M BH = 2.4 ± 0.6 × 10 9 M ⊙ and M BH = 2.9 ± 0.3 × 10 9 M ⊙ , respectively. Neither model can account for the non-axisymmetric stellar velocity features present in the IFS data.

Evidence of the Triaxial Structure of ^{129}Xe at the Large Hadron Collider.

The interpretation of the emergent collective behavior of atomic nuclei in terms of deformed intrinsic shapes is at the heart of our understanding of the rich phenomenology of their structure, ranging from nuclear energy to astrophysical applications across a vast spectrum of energy scales. A new window into the deformation of nuclei has been recently opened with the realization that nuclear collision experiments performed at high-energy colliders, such as the CERN Large Hadron Collider (LHC), enable experimenters to identify the relative orientation of the colliding ions in a way that magnifies the manifestations of their intrinsic deformation. Here we apply this technique to LHC data on collisions of ^{129}Xe nuclei to exhibit the first evidence of nonaxiality in the ground state of ions collided at high energy. We predict that the low-energy structure of ^{129}Xe is triaxial (a spheroid with three unequal axes) and show that such deformation can be determined from high-energy data. This result demonstrates the unique capabilities of precision collider machines such as the LHC as new means to perform imaging of the collective structure of atomic nuclei.

Intrinsic alignments in IllustrisTNG and their implications for weak lensing: Tidal shearing and tidal torquing mechanisms put to the test

ABSTRACT Accurate measurements of the cosmic shear signal require a separation of the true weak gravitational lensing signal from intrinsic shape correlations of galaxies. These ‘intrinsic alignments’ of galaxies originate from galaxy formation processes and are expected to be correlated with the gravitational field through tidal processes affecting the galaxies, such as tidal shearing for elliptical galaxies and tidal torquing for spiral galaxies. In this study, we use morphologically selected samples of elliptical and spiral galaxies from the illustrisTNG simulation at z = 0 and z = 1 to test the commonly employed linear (tidal shearing) and quadratic (tidal torquing) models for intrinsic alignments. We obtain local measurements of the linear and quadratic alignment parameters, including corrections for large-scale anisotropies of the cosmologically small simulation volume, and study their dependence on galaxy and environmental properties. We find a significant alignment signal for elliptical galaxies (linear model), that increases with mass and redshift. Spiral galaxies (quadratic model), on the other hand, exhibit a significant signal only for the most massive objects at z = 1. We show the quadratic model for spiral galaxies to break down at its fundamental assumptions, and simultaneously obtain a significant signal of spiral galaxies to align according to the linear model. We use the derived alignment parameters to compute intrinsic alignment spectra and estimate the expected contamination in the weak lensing signal obtained by Euclid.

Markerless registration approach using dynamic touchable region model.

Markerless registration is required for image-guided surgery; it has limited accuracy due to the ambiguity of the correspondence point set. In this study, we proposed a registration framework to improve registration accuracy for markerless registration using a dynamic touchable region model (DTRM). The DTRM is defined using the geometric characteristics of the surface around the fiducial area using Intrinsic Shape Signature keypoints. The new registration procedure, which combines the DTRM with iterative closest point-based registration (ICDTP) was implemented and verified with phantom experiments for a single-user and multi-user study. The ICDTP registration framework provides improved performance over the paired-point registration for surgeries, where it is inappropriate to construct the corresponding positions with adhesive fiducial markers. The proposed method can be an alternative approach for image-guided surgery in operations for which itis not appropriate to set up markers for registration.

Triaxial Orbit-based Dynamical Modeling of Galaxies with Supermassive Black Holes and an Application to Massive Elliptical Galaxy NGC 1453

Abstract Most stellar-dynamical determinations of the masses of nearby supermassive black holes (SMBHs) have been obtained with the orbit superposition technique under the assumption of axisymmetry. However, few galaxies—in particular massive early-type galaxies—obey exact axisymmetry. Here we present a revised orbit superposition code and a new approach for dynamically determining the intrinsic shapes and mass parameters of triaxial galaxies based on spatially resolved stellar kinematic data. The triaxial TriOS code described here corrects an error in the original van den Bosch et al. code that gives rise to incorrect projections for most orbits in triaxial models and can significantly impact parameter search results. The revised code also contains significant improvements in orbit sampling, mass constraints, and run time. Furthermore, we introduce two new parameter-searching strategies—a new set of triaxial shape parameters and a novel grid-free sampling technique—that together lead to a remarkable gain in efficiency in locating the best-fit model. We apply the updated code and search method to NGC 1453, a fast-rotating massive elliptical galaxy. A full 6D parameter search finds p = b / a = 0.933 − 0.015 + 0.014 and q = c/a = 0.779 ± 0.012 for the intrinsic axis ratios and T = 0.33 ± 0.06 for the triaxiality parameter. Despite the deviations from axisymmetry, the best-fit SMBH mass, stellar mass-to-light ratio, and dark matter enclosed mass for NGC 1453 are consistent with the axisymmetric results. More comparisons between axisymmetric and triaxial modeling are needed before drawing general conclusions.