The Selection of Simple Model Atoms for Calculations of Electron Density in Nonequilibrium, Low Temperature Cs Plasmas
Simple model atoms for calculations of electron density in nonequilibrium, low temperature cesium plasmas
Dugan, J. V., Jr.↗
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Results for “Temperature model”
Search indexed NASA NTRS and DOE OSTI research on propulsion, heat transfer, battery materials and energy systems. Follow report and document links to the original sources.
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Biaxial constitutive modelling and testing of a single crystal superalloy at elevated temperatures
A viscoplastic constitutive model for single crystal superalloys is developed from crystallographic slip theory. The model is applied to the tension and torsion deformation behavior of the single crystal superalloy PWA 1480 at 871 C (1600 F). Both octahedral and cube slip behavior are needed to model the deformation behavior of single crystal superalloys at elevated temperature.
Walker, K. P.↗
Can Simple Machine Learning Tools Extend and Improve Temperature-Based Methods to Infer Streambed Flux?
Temperature-based methods have been developed to infer 1D vertical exchange flux between a stream and the subsurface. Current analyses rely on fitting physically based analytical and numerical models to temperature time series measured at multiple depths to infer daily average flux. These methods have seen wide use in hydrologic science despite strong simplifying assumptions including a lack of consideration of model structural error or the impacts of multidimensional flow or the impacts of transient streambed hydraulic properties. We performed a “perfect-model experiment” investigation to examine whether regression trees, with and without gradient boosting, can extract sufficient information from model-generated subsurface temperature time series, with and without added measurement error, to infer the corresponding exchange flux time series at the streambed surface. Using model-generated, synthetic data allowed us to assess the basic limitations to the use of machine learning; further examination of real data is only warranted if the method can be shown to perform well under these ideal conditions. We also examined whether the inherent feature importance analyses of tree-based machine learning methods can be used to optimize monitoring networks for exchange flux inference.
54 ENVIRONMENTAL SCIENCES↗
Near-infrared spectroscopy of the Y0 WISEP J173835.52+273258.9 and the Y1 WISE J035000.32-565830.2: the importance of non-equilibrium chemistry
We present new near-infrared spectra, obtained at Gemini Observatory, for two Y dwarfs: WISE J035000.32−565830.2 (W0350) and WISEP J173835.52+273258.9 (W1738). A FLAMINGOS-2 R = 540 spectrum was obtained for W0350, covering 1.0<λ μm < 1.7, and a cross-dispersed Gemini near-infrared spectrograph R = 2800 spectrum was obtained for W1738, covering 0.993–1.087 μm, 1.191–1.305 μm, 1.589–1.631 μm, and 1.985–2.175 μm, in four orders. We also present revised YJH photometry for W1738, using new NIRI Y and J imaging, and a re-analysis of the previously published NIRI H-band images. We compare these data, together with previously published data for late-T and Y dwarfs, to cloud-free models of solar metallicity, calculated both in chemical equilibrium and with disequilibrium driven by vertical transport. We find that for the Y dwarfs, the non-equilibrium models reproduce the near-infrared data better than the equilibrium models. The remaining discrepancies suggest that fine-tuning the CH{sub 4}/CO and NH{sub 3}/N{sub 2} balance is needed. Improved trigonometric parallaxes would improve the analysis. Despite the uncertainties and discrepancies, the models reproduce the observed near-infrared spectra well. We find that for the Y0, W1738, T{sub eff}=425±25 K, and log g=4.0±0.25, and for the Y1, W0350, T{sub eff}=350±25 K, and log g=4.0±0.25. W1738 may be metal-rich. Based on evolutionary models, these temperatures and gravities correspond to a mass range for both Y dwarfs of 3–9 Jupiter masses, with W0350 being a cooler, slightly older, version of W1738; the age of W0350 is 0.3–3 Gyr, and the age of W1738 is 0.15–1 Gyr.
79 ASTRONOMY AND ASTROPHYSICS↗
Temperature structure in the Perseus cluster core observed with Hitomi*
The present paper investigates the temperature structure of the X-ray emitting plasma in the core of the Perseus cluster using the 1.8–20.0 keV data obtained with the Soft X-ray Spectrometer (SXS) onboard the Hitomi Observatory. A series of four observations were carried out, with a total effective exposure time of 338 ks and covering a central region ~7' in diameter. The SXS was operated with an energy resolution of ~5 eV (full width at half maximum) at 5.9 keV. Not only fine structures of K-shell lines in He-like ions but also transitions from higher principal quantum numbers are clearly resolved from Si through Fe. This enables us to perform temperature diagnostics using the line ratios of Si, S, Ar, Ca, and Fe, and to provide the first direct measurement of the excitation temperature and ionization temperature in the Perseus cluster. The observed spectrum is roughly reproduced by a single temperature thermal plasma model in collisional ionization equilibrium, but detailed line ratio diagnostics reveal slight deviations from this approximation. In particular, the data exhibit an apparent trend of increasing ionization temperature with increasing atomic mass, as well as small differences between the ionization and excitation temperatures for Fe, the only element for which both temperatures can be measured. The best-fit two-temperature models suggest a combination of 3 and 5 keV gas, which is consistent with the idea that the observed small deviations from a single temperature approximation are due to the effects of projection of the known radial temperature gradient in the cluster core along the line of sight. Comparison with the Chandra/ACIS and the XMM-Newton/RGS results on the other hand suggests that additional lower-temperature components are present in the ICM but not detectable by Hitomi SXS given its 1.8–20 keV energy band.
79 ASTRONOMY AND ASTROPHYSICS↗
Temperature Structure in the Perseus Cluster Core Observed with Hitomi
The present paper investigates the temperature structure of the X-ray emitting plasma in the core of the Perseus cluster using the 1.8-20.0 keV data obtained with the Soft X-ray Spectrometer (SXS) onboard the Hitomi Observatory. A series of four observations were carried out, with a total effective exposure time of 338 ks and covering a central region _ 7′ in diameter. The SXS was operated with an energy resolution of _5 eV (full width at half maximum) at 5.9 keV. Not only fine structures of K-shell lines in He-like ions but also transitions from higher principal quantum numbers are clearly resolved from Si through Fe. This enables us to perform temperature diagnostics using the line ratios of Si, S, Ar, Ca, and Fe, and to provide the first direct measurement of the excitation temperature and ionization temperature in the Perseus cluster. The observed spectrum is roughly reproduced by a single temperature thermal plasma model in collisional ionization equilibrium, but detailed line ratio diagnostics reveal slight deviations from this approximation. In particular, the data exhibit an apparent trend of increasing ionization temperature with increasing atomic mass, as well as small differences between the ionization and excitation temperatures for Fe, the only element for which both temperatures can be measured. The best-fit two-temperature models suggest a combination of 3 and 5 keV gas, which is consistent with the idea that the observed small deviations from a single temperature approximation are due to the effects of projection of the known radial temperature gradient in the cluster core along the line of sight. Comparison with the Chandra/ACIS and the XMM-Newton/RGS results on the other hand suggests that additional lower-temperature components
Aharonian, Felix↗
Predicting Fueled Experiment Swelling and Thermal Expansion Using STAR-CCM+
An experiment being designed at Idaho National Laboratory (INL) has an unusual temperature requirement. The surface temperature must remain above 300 C over the irradiation lifetime. The fuel in this experiment is composed of uranium-nitride (UN) tri-structural-isotropic (TRISO) particles encased in a cylindrical, SiC matrix. Increased swelling of SiC at lower temperatures is the basis for this lower temperature limit. For a typical thermal analysis, the focus is on some upper limit of the center-line temperature. This tends to be a more straight-forward process where the analyst makes a series of worst-case assumptions and demonstrates that the experiment - even under those conditions - cannot exceed the maximum temperature. The model used to ensure the experiment will always have a surface temperature in excess of 300 C has been developed using STAR-CCM+. Notable properties of the simulation include - Full 3D fluid and heat transfer modeling; - Geometry input taken directly from design engineer's CAD files; - Fuel swelling and thermal conductivity as functions of displacements per atom (DPA) and temperature; - Radial thermal expansion of fuel, rodlet, and capsule; - Jump gap and surface roughness implemented using equations from BISON. These things together have yielded a model with sufficient detail to predict minimum surface temperatures with the greatest precision attainable with available data. The only notable approximation is the zirconia insulator, which will actually be a sphere. This particular shape was chosen to expedite meshing, while maintaining a realistic degree of physical contact with adjacent components. Given temperature and irradiation dependent data for thermal conductivity and fuel swelling of a SiC matrix, it was possible to perform an in-depth thermal analysis to find an optimal configuration of radial gas gaps. Of greatest importance was that the fuel surface temperature remain above 300 C. This criteria was met with a healthy margin, even when considering machining tolerances of ±1 mil on the gas gaps.
11 NUCLEAR FUEL CYCLE AND FUEL MATERIALS↗
A quantitative model of plasma in Neptune's magnetosphere
A model encompassing plasma transport and energy processes is applied to Neptune's magnetosphere. Starting with profiles of the neutral densities and the electron temperature, the model calculates the plasma density and ion temperature profiles. Good agreement between model results and observations is obtained for a neutral source of 5 x 10 exp 25/s if the diffusion coefficient is 10 exp -8 L3R(N)/2s, plasma is lost at a rate 1/3 that of the strong diffusion rate, and plasma subcorotates in the region outside Triton.
Richardson, John D.↗
The analysis of fatigue crack growth mechanism and oxidation and fatigue life at elevated temperatures
Two quantitative models based on experimentally observed fatigue damage processes have been made: (1) a model of low cycle fatigue life based on fatigue crack growth under general-yielding cyclic loading; and (2) a model of accelerated fatigue crack growth at elevated temperatures based on grain boundary oxidation. These two quantitative models agree very well with the experimental observations.
Liu, H. W.↗
A model for analysis of the temperature field downstream of a heated jet injected into an isothermal crossflow at an angle of 90 deg
The temperature distribution downstream of a heated jet entering an isothermal crossflow at an angle of 90 deg is predicted using two conduction models with energy sources above the point of injection, in one case a point source and in the second a line source. The models use effective turbulent diffusivities that are determined empirically from previous measurements. Temperatures predicted by the models are compared to experimental results.
Eriksen, V. L.↗
A theoretical model for the cross spectra between pressure and temperature downstream of a combustor
A theoretical model developed to calculate pressure-temperature cross spectra, pressure spectra, temperature spectra and pressure cross spectra in a ducted combustion system is presented. The model assumes the presence of a fluctuating-volumetric-heat-release-rate disk source and takes into account the spatial distribution of the steady-state volumetric-heat flux. Using the model, pressure, velocity, and temperature perturbation relationships can be obtained. The theoretical results show that, at a given air mass flow rate, the calculated pressure-temperature cross spectra phase angle at the combustor exit depends on the model selected for the steady-state volumetric-heat flux in the combustor. Using measurements of the phase angle, an appropriate source region model was selected. The model calculations are compared with the data. The comparison shows good agreement and indicates that with the use of this model the pressure-temperature cross spectra measurements provide useful information on the physical mechanisms active at the combustion noise source.
Miles, J. H.↗
Glass Transition Temperature- and Specific Volume- Composition Models for Tellurite Glasses
This report provides models for predicting composition-properties for tellurite glasses, namely specific gravity and glass transition temperature. Included are the partial specific coefficients for each model, the component validity ranges, and model fit parameters.
36 MATERIALS SCIENCE↗
Modeling of a High-Temperature-Serpentine External Tubular Receiver Using Supercritical CO 2
This paper describes the modelling and design of an external receiver using supercritical CO 2 as the heat transfer fluid that can reach up to 700 °C outlet temperature with ~85% thermal efficiency. The internal pressure of the tubes is 20 MPa. The receiver tubes are arranged in a serpentine fashion and are coated with Pyromark 2500. Analyses were performed to evaluate the thermal efficiency of the receiver as a function of incidence angle of the incident radiation. Two different radiation models, discrete ordinates and surface-to-surface ray tracing, were used in the computational fluid dynamics model (ANSYS FLUENT). The receiver thermal efficiency ranged from 75% for incidence angles of 80 degrees to 88% for near-normal incidence angles of 10 degrees.
54 ENVIRONMENTAL SCIENCES↗
Incorporating variability in simulations of seasonally forced phenology using integral projection models
Phenology models are becoming increasingly important tools to accurately predict how climate change will impact the life histories of organisms. We propose a class of integral projection phenology models derived from stochastic individual-based models of insect development and demography. Our derivation, which is based on the rate-summation concept, produces integral projection models that capture the effect of phenotypic rate variability on insect phenology, but which are typically more computationally frugal than equivalent individual-based phenology models. We demonstrate our approach using a temperature-dependent model of the demography of the mountain pine beetle (Dendroctonus ponderosae Hopkins), an insect that kills mature pine trees. This work illustrates how a wide range of stochastic phenology models can be reformulated as integral projection models. Due to their computational efficiency, these integral projection models are suitable for deployment in large-scale simulations, such as studies of altered pest distributions under climate change.
Goodsman, Devin W.↗
Evidence of the AMOC interdecadal mode related to westward propagation of temperature anomalies in CMIP5 models
Not provided.
Meteorology & Atmospheric Sciences↗