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38 results for “binary systems”
Dataset for "DEM-CFD analysis of swelling behaviours of binary particle systems with a microscopic diffusion model"
<p>This dataset contains both numerical simulation data and experimental data describing the swelling behaviour of binary particle systems. Detailed study on the swelling behaviour is presented in a journal paper entitled "DEM-CFD analysis of swelling behaviours of binary particle systems with a microscopic diffusion mode". We provide all the essential data in a single excel file with the description below:</p> <p>Dataset 1- Evolution of the height of the particle bed obtained from experiments and simulations (used in Fig.6 of the associated paper): Experimental data for the measured hight and associated standard deviation at various time, as well as the numerical data.</p> <p>Dataset 2 - Evolutions of the normalised average radius r/r_0 (used in Fig.7a) and the coefficient of variation CV (used in Fig.7b) for SAP particles obtained from DEM-CFD simulations.</p> <p>Dataset 3 - Radial distribution Functions (RDFs) for (Fig.9a) SAP particles and (Fig.9b) POM particles at different time instants.</p> <p>Dataset 4 - Positions of POM particles projected into the x-y plane at different time instants (the red dots are particle centres), (a) t = 0 min; (b) t = 3 min; (c) t = 6 min; (d) t = 10 min.</p> <p>Dataset 5 - Evolution of Lacey mixing index for the binary particles during the swelling process.</p> <p>Dataset 6 - Average normal stress distribution of particles in x-y and x-z planes at t = 2 min.</p> <p>DataSet 7 - Velocity vectors of particles projected in x-z planes at different time instants: (a) t = 1 min; (b) t= 2 min (Data for Fig.13)</p> <p>Dataset 8 - Positions of POM particles projected into x-y plane at time t= 10 min (the red dots are particle centres) with different coefficient of frictions (a) μ=0.1; (b) μ=0.2; (c) μ=0.3; (d) μ=0.4; (e) μ=0.5.(Data for Fig.15)</p> <p>Dataset 9 - RDFs for POM particles at time t= 10 min with different coefficients of friction.(Data for Fig.16)</p>
Properties of binary systems in a one-dimensional approximation
<p>We present numerically obtained tables of properties of stars in a binary system as a function of the effective potential: volume-equivalent radii of the equipotential surfaces, effective accelerations averaged over the same equipotential surfaces and the properties of the L<sub>1</sub> plane cross-sections. The tables are obtained for binaries where the ratios of the primary star mass to the companion star mass are from 10<sup>-6</sup> to 10<sup>5</sup> and include equipotential surfaces up to the star's outer Lagrangian point. We supply a sample code showing how to use our tables to get the average effective accelerations in one-dimensional stellar codes.</p> <p>Updates will be available at <a href="https://github.com/AliPourmand/1D_binary_star_properties">https://github.com/AliPourmand/1D_binary_star_properties</a>. Paper describing the tables can be found on ApJ, <strong>DOI</strong> 10.3847/1538-4357/acd4c1, https://iopscience.iop.org/article/10.3847/1538-4357/acd4c1 If you make use of the provided tables or the code, we ask you to cite the paper (and zenodo deposit if such reference is allowed).</p>
Yields from paper: ALUMINIUM-26 FROM MASSIVE BINARY STARS III. BINARY STARS UP TO CORE-COLLAPSE AND THEIR IMPACT ON THE EARLY SOLAR SYSTEM
<p>================================================================================<br> Title: Aluminium-26 From Massive Binary Stars III: BINARY STARS UP TO CORE-COLLAPSE AND THEIR IMPACT ON THE EARLY SOLAR SYSTEM<br> Authors: Brinkman H.E., Doherty C.L., Pignatari M., Pols, O. R., Lugaro M.<br> ================================================================================<br> Description of contents: A .tar.gz package containing 12 files with the complete set<br> of yields from the models presented in this paper. Each file contains one primary mass,<br> e.g., Yields10Msun contains the yields for the binary systems with a 10Msun primary.<br> The second line in each file has the periods.<br> ================================================================================</p>
Photometry of outer Solar System objects from the Dark Energy Survey I: photometric methods, light curve distributions and trans-Neptunian binaries - data release
<p>This repository contains the full data release for the 814 outer Solar System objects found in the Dark Energy Survey.</p> <p>A full description of the object search is described in <a href="http://(https://ui.adsabs.harvard.edu/abs/2022ApJS..258...41B/abstract">Bernardinelli et al (2022)</a>, and a full description of the photometric processing is described in<a href="https://ui.adsabs.harvard.edu/abs/2023arXiv230403017B/abstract"> Bernardinelli et al (2023)</a>. If you use these files, we ask you to cite the corresponding papers.</p> <p>The FITS table `y6_des_tnos_color.fits` contains both the orbital elements and the colors for each object. The full description of the orbital element information is given in Table 3 of <a href="https://ui.adsabs.harvard.edu/abs/2022ApJS..258...41B/abstract">Bernardinelli et al (2022</a>). In addition to these, the table also includes the mean absolute magnitudes in each band, as well as mean <span class="math-tex">\((g-r, r-i, r-z)\)</span> colors and their corresponding covariance matrix, and the 68% confidence interval for the lightcurve amplitude.</p> <p>Inside the `fluxes` directory, the complete photometric record for each object is included in a `hdf5` file (for each object), and the MCMC chains for their fluxes and LCAs. The three Jupyter Notebooks included in the `notebooks` directory explains the columns and how to use these files to reproduce the results of the paper. Inside this directory there are also additional files needed to reproduce the code.</p> <p>The `binary` directory has the MCMC chains for their mutual orbits (in `.npy` files), as well as the astrometric and photometric record for the binary measurements. Another `README` file is included in that directory with a detailed explanation.</p>
Data from: A pulsar-helium star compact binary system formed by common envelope evolution
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The eclipsing binary systems with delta Scuti component. AB Cas
<p>A set of inlists for MESA v12115, used to compute a grid of binary evolutionary tracks used in the paper "The eclipsing binary systems with delta Scuti component. AB Cas".</p>
Simulated astrometric binary systems
<p>Simulated systems analyzed in Penoyre, Belokurov & Evans 2022.</p> <p>As detailed in the paper we generate 100,000 random binary configurations with 100 pc and simulate each as:</p> <ul> <li>a single star (l=q=0)</li> <li>a stellar binary (l and 1 generated by drawing a second random star, l<1 always)</li> <li>a solar mass black hole (l=0)</li> <li>a three solar mass black hole</li> <li>a ten solar mass black hole</li> </ul>
Equipment Design for a Small Binary System Power Plant Using Geothermal Heating Fluid A Case Study
<p>This material has presented on 2nd International Conference on Advanced Research in Engineering and Technology in October 25, 2023.</p>
Inlists used for studying the astrophysical properties of the Sirius binary system
<p>Using mesa-r23.05.1 a study of the sirius system was performed, both as a non-interacting binary, as well as test suites that take sirius b up until the wd cooling phases in an attempt to better understand the age of the system and the limits of the progenitor mass. Additionally, we hope to put constraints on the temperature, luminosity, and white dwarf mass by comparing this simulation to HST data. Lastly, we use these models to calculate an initial to final mass relation for the system.</p> <p>The inlists used have been included as well as some mod files for different metallicities and initial masses. It is split into three sections pertaining to the binary suite, and single star evolutions where we create carbon and oxygen white dwarfs for lower initial masses of sirius b, as well as a test suite that creates a neon oxygen white dwarf for larger initial masses.</p> <p>The mesasdk version is from July of last year (version 23.7.3)</p>
Data for "Supervised machine learning methods for crystal structure prediction of the binary Cs-Te system"
<p>Crystal structures, high-throughput calculations and trained machine learning models presented in the paper "Supervised machine learning methods for crystal structure prediction of the binary Cs-Te system".</p> <ul> <li><em>crystal_datasets </em>contains the input/output data sets of crystal structures for high-throughput calculations and ML models.</li> <li><em>aiida_ht_calculations </em>contains the data regarding the high-throughput DFT calculations.</li> <li><em>ml_models</em> contains the trained ML models.</li> </ul> <p>Eeach zip-archive contains a jupyter-notebook examplifying how the data can be accessed and reused.</p>
Iron Bonding with Light Elements: Implications for Planetary Cores Beyond the Binary System
<p>X-ray Absorption Spectroscopy and DFT calculation dataset for Iron alloys at high pressures. <br><br></p> <p><strong>Abstract: </strong>Light element alloying in iron is required to explain density deficit and seismic wave velocities in Earth’s core. However, the light element composition of the Earth’s core seems hard to constrain as nearly all light element alloying would reduce the density and sound velocity (elastic moduli). The alloying light elements include oxidizing elements like oxygen and sulfur, and reducing elements like hydrogen and carbon, yet their chemical effects in alloy system are less discussed. Moreover, Fe-X-ray Absorption Near Edge Structure (Fe-XANES) fingerprints have been studied for silicate materials with ferrous and ferric ions, while not many X-ray absorption spectroscopy (XAS) studies have focused on iron alloys, especially at high pressures. To investigate the bonding nature of iron alloys in planetary interiors, we presented X-ray absorption spectroscopy of iron-nitrogen and iron-carbon alloys at high pressure up to 50 GPa. Together with existing literature on iron-carbon, -hydrogen alloys, we analyzed their edge positions and found no significant difference of degree of oxidation among these alloys. Pressure effects on edge positions were also found negligible. Our theoretical simulation of the valence state of iron, alloyed with S, C, O, N, P also showed nearly unchanged behavior under pressures up to 300 GPa. This indicates the high pressure bonding of iron alloyed with light elements closely resembles bonding at the ambient conditions. We suggest that the chemical properties of light elements constrain which ones can coexist within iron alloys.<span> </span></p>
Binary Approach to Ternary Cluster Expansions: NO–O–Vacancy System on Pt(111)
<p>Cluster expansions (CEs) provide an exact framework for representing the configurational energy of interacting adsorbates at a surface. Coupled with Monte Carlo methods, they can be used to predict both equilibrium and dynamic processes at surfaces. In this work, we propose a three-binary-to-single-ternary (TBST) fitting procedure, in which a ternary CE is approximated as a linear combination of the three binary CEs (O–vac, NO–vac, and NO–O) obtained by fitting to the three binary legs. We first construct a full ternary CE by fitting to a database of density functional theory (DFT) computed energies of configurations across a full range of adsorbate configurations and then construct a second ternary using the TBST approach. We compare two approaches for the NO–O–vacancy system on the (111) surface of Pt, a system of relevance to the catalytic oxidation of NO. We find that the TBST model matches the ternary CE to within 0.018 eV/site across a wide range of configurations. Further, surface coverages and NO oxidation rates extracted from Monte Carlo simulations show that the two models are qualitatively consistent over the range of conditions of practical interest.</p>
Effects of Rotationally Induced Mixing in Compact Binary Systems with Low-mass Secondaries and in Single Solar-type Stars
<p>MESA inlists associated with <a href="https://ui.adsabs.harvard.edu/#abs/2012ApJ...755...95C/abstract">Chatzopoulos et al. (2012)</a>. MESA version 3647.</p> <p>Publication DOI: <a href="https://www.doi.org/10.1088/0004-637X/755/2/95">10.1088/0004-637X/755/2/95</a></p>
Data for 'SPH modelling of wind-companion interactions in eccentric AGB binary systems'
<p>Additional material to "Malfait et al. 2021, SPH modelling of wind-companion interactions in eccentric AGB binary systems": <a href="https://ui.adsabs.harvard.edu/link_gateway/2021A&A...652A..51M/arxiv:2107.01074" target="_blank" rel="noreferrer noopener">arXiv:2107.01074</a></p> <p>This contains input files and final output dumps of the Phantom simulations of this paper, and additional movies of 4 of the simulations.</p> <p>The code used to perform the simulations is available at: <a href="https://github.com/danieljprice/phantom">https://github.com/danieljprice/phantom.</a></p> <p>Splash (<a href="https://github.com/danieljprice/splash">https://github.com/danieljprice/splash</a> ) and Plons (<a href="https://github.com/Ensor-code/plons">https://github.com/Ensor-code/plons</a> ) were used to create figures and plots from this data.</p>
Tagged formatted datasets for 'Genetically Optimized Massively Parallel Binary Neural Networks for Intrusion Detection Systems'
<p>Tagged formatted datasets used in 'Genetically Optimized Massively Parallel Binary Neural Networks for Intrusion Detection Systems' T.Murovič, A.Trost.</p>
Dynamical Masses of Selected Orbital Binary Systems
Orbital binary stars are essential objects for determining dynamical and physical properties of stars through a combined analysis of photometric and astrometric data. The authors have compiled a set of orbital binaries with known trigonometric parallaxes and orbits of high quality, using data from current versions of the Observatorio Astronomico Ramon Maria Aller Catalog (OARMAC) of Orbits and Ephemerides of Visual Double Stars (Docobo et al. 2001, AcA, 51, 353) and the Sixth Catalog of Orbits of Visual Binary Stars (ORB6: Mason and Hartkopf 2007, IAUS 240, 575; Hartkopf et al. 2001, AJ, 122, 3472), as well as including updated information from the Washington Double Star (WDS) Catalog and SIMBAD. They constructed distributions of orbital binaries of the dynamical mass, period, semi-major axis, and eccentricity of systems, which characterize the set. Some problems related to the parametrization of orbital binaries are also discussed in the paper. To compile the orbit list, the authors combined data from both OARMAC and ORB6. At this stage, they maintained systems without parallaxes, but removed systems without a period or semi-major axis. The resulting list contained 3139 orbits for 2278 pairs: 1588 pairs have a single orbit, 548 pairs have two orbits, 120 pairs have three orbits, 19 pairs have four orbits, one pair has five orbits, and two pairs have seven orbits. Table 1 in the reference paper (not part of this HEASARC table) contains a compiled set of 3139 orbit solutions for visual binary stars. Separate entries are provided for different pairs in multiple systems. Several solutions per pair are possible. Each entry includes main orbital elements (Semi-major axis, period, eccentricity with corresponding uncertainties), indication of multiplicity and number of solutions, as well as visual magnitudes, spectral classes of the components, parallax and interstellar extinction estimate. Table 2 in the reference paper (on which this HEASARC table is based) contains a refined set of 652 solely binary systems with reliable orbits and determined parallaxes. One entry in this table corresponds to one system. Three mass estimates are provided: (1) The dynamical mass with its uncertainty derived from Kepler's third law and its trigonometric parallax, (2) a photometric mass estimated from the visual magnitudes, parallax and mass-luminosity relation, and (3) a spectroscopic mass based on the mass-spectrum relation introduced by Straizys and Kuriliene (1981, Ap&SS, 80, 353). Also provided for each system are the main orbital elements, the parallax, and the component magnitudes and spectral types. This table was created by the HEASARC in October 2014 based on the list of orbital binaries given in <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/546/A69">CDS Catalog J/A+A/546/A69</a> file table2.dat. Note that this table does not include the information on individual orbits which given listed in file table1.dat of this CDS catalog. This is a service provided by NASA HEASARC .
Double knock-in pig models with elements of binary Tet-on and phiC31 intergrase systems for controllable and switchable gene expression
GEO Series GSE176519. Sus scrofa. 18 samples. Type: Expression profiling by high throughput sequencing.
Data for "A binary system in the S cluster close to the supermassive black hole Sagittarius A*"
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