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47 results for “equation of state”
Equation of state for simulations of core-collapse supernovae and neutron-star mergers
<p>We construct a new equation of state (EOS) for numerical simulations of core-collapse supernovae and neutron-star mergers based on an extended relativistic mean-field model with a small symmetry energy slope L, which is compatible with both experimental nuclear data and recent observations of neutron stars. The new EOS table (EOS4) based on the extended TM1 (TM1e) model with L=40 MeV is designed in the same tabular form as the commonly used Shen EOS (EOS2) based on the original TM1 model with L=110.8 MeV. This is convenient and useful for performing numerical simulations and examining the influences of symmetry energy and its density dependence on astrophysical phenomena. </p> <p> </p>
Ensembles for neutron-star-matter equation-of-state interpolations
<p>Ensembles for neutron-star-matter equation-of-state interpolations to reproduce the figures in arXiv:2303.11356</p>
A Nuclear Equation of State Inferred from Stellar r-Process Abundances: Data
<p>This repository contains the raw MCMC posteriors as H5 files for the three cases presented in "A Nuclear Equation of State Inferred from Stellar <em>r</em>-Process Abundances" (<a href="https://ui.adsabs.harvard.edu/abs/2021arXiv211006432H/abstract">Holmbeck et al., arXiv:2110.06432</a>).</p> <p>Also included are Python scripts with a variety of functions to read the H5 files and interpret the data with <a href="https://git.ligo.org/lscsoft/lalsuite">LALSuite</a>. These include:</p> <ul> <li>reading the data contained in the H5 file (likelihood, acceptance, and values for each MCMC step)</li> <li>generating a corner plot of the data</li> <li>finding the maximum likelihood in the posterior distribution</li> <li>calculating a neutron star mass-radius curve for a posterior EOS</li> <li>calculating pressure and density for a posterior EOS</li> <li>calculating observables (M_TOV, R_1.4, and L) associated with an EOS</li> </ul> <p>The scripts are written for Python3 compatibility and depend on:</p> <ul> <li><a href="https://pypi.org/project/lalsuite/">lalsuite</a></li> <li><a href="https://docs.h5py.org/en/stable/">h5py</a></li> <li><a href="https://numpy.org/">numpy</a></li> <li><a href="https://scipy.org/">scipy</a></li> <li><a href="https://matplotlib.org/">matplotlib</a></li> <li><a href="https://corner.readthedocs.io/en/latest/">corner</a></li> </ul> <p>For more information and how to use these scripts, see the comments in `example.py` or contact Erika Holmbeck.</p> <p>If any of our posterior samples are used in your work, we ask that you appropriately cite this repository and the original paper (<a href="https://ui.adsabs.harvard.edu/abs/2021arXiv211006432H/abstract">Holmbeck et al., arXiv:2110.06432</a>).</p>
Supernova Neutrino Light Curves from Proto-Neutron Star Cooling with Various Nuclear Equation of State
<p>We present the model spectra of neutrinos emitted from proto-neutron star (PNS) cooling used in Nakazato et al., <a href="https://doi.org/10.3847/1538-4357/ac3ae2">Astrophys. J. <strong>925</strong> (2022) 98</a>, <a href="https://arxiv.org/abs/2108.03009">arXiv:2108.03009 [astro-ph.HE]</a>. So as to obtain the time evolution of neutrino spectra, PNS cooling simulations are performed with use of four nuclear equation of state (EOS) models and eight PNS cooling models with different initial conditions are involved for each EOS. The format of the spectral data is the same with that of <a href="http://asphwww.ph.noda.tus.ac.jp/snn/">Supernova Neutrino Database</a>. For the details, see readme.pdf</p>
Multi-objective optimization of equation of state molecular parameters: SAFT-VR Mie models for water
<p>Supporting document containing information on the Pareto points and thermodynamic calculations.</p>
EXAMPLE: Lattice-based equation of state tables with three conserved charges (BSQ)
<p>These table is intended to provide an example format of the equation of state expected for the CCAKE hydrodynamic code which propagates conserved charge densities for baryon number <span class="math-tex">\(B\)</span>, net strangeness <span class="math-tex">\(S\)</span>, and electric charge <span class="math-tex">\(Q\)</span>. They are included primarily for demonstration purposes and no claim is made as to the accuracy of their contents.</p>
Thermodynamic characterization of the (H2 + C3H8) system significant for the hydrogen economy: Experimental (p, rho, T) determination and equation of-state modelling
<p>File: 2023_IJHE_Manuscript_repository.docx</p> <p>This is an author-created, un-copyedited version of an article accepted for publication in the International Journal of Hydrogen Energy (2023, 48 (23), 8645-8667). The editor of the Journal is not responsible for any errors or omissions in this version of the manuscript or any version derived from it. The definitive publisher-authenticated, Open-Access version is available online at: https://doi.org/10.1016/j.ijhydene.2022.11.170<br><br>File: 2023_IJHE_Results_Repository.xlsx</p> <p>This is the MS Excel data file of the paper. </p> <p> </p> <p> </p>
A three-parameter characterization of neutron stars' mass-radius relation and equation of state
<p>A dataset for the paper <a href="https://arxiv.org/abs/2404.17647" target="_blank" rel="noopener">A three-parameter characterization of neutron stars' mass-radius relation and equation of state</a></p> <p>See<strong><em> Readme</em></strong> file for details.</p> <p>We aslo provide the <a href="https://github.com/pshternin/unicorrns" target="_blank" rel="noopener">unicorrns</a> python package wich allows to employ the results of our paper in a convenient way.</p> <p>The fitting subroutibe for NS mass and radius data analysis used in the paper is available at <a href="https://github.com/pshternin/nsmr2eos" target="_blank" rel="noopener">https://github.com/pshternin/nsmr2eos</a></p>
Equation of State, Structure, and Transport Properties of Iron Hydride Melts at Planetary Interior Conditions dataset
<p>Datasets from <a href="https://doi.org/10.1029/2024JE008525">https://doi.org/10.1029/2024JE008525</a></p> <p>"Equation of State, Structure, and Transport Properties of Iron Hydride Melts at Planetary Interior Conditions"</p> <p>Emma R. Stoutenburg1, Razvan Caracas2, Natalia V. Solomatova3, and Andrew J. Campbell1</p> <p>1Department of the Geophysical Sciences, University of Chicago, Chicago, IL, USA, 2 Université Paris Cité, Institut de Physique du Globe de Paris, CNRS, 1 rue Jussieu, Paris, France, 3CNRS, Ecole Normale Supérieure de Lyon, Laboratoire de Géologie de Lyon LGLTPE UMR5276, Centre Blaise Pascal, Lyon, France</p> <p>--- </p> <p><em>Please make sure you download data from the 30 October, 2024 version. </em> </p> <p>--- </p> <p>ds01.xlsx</p> <p>Contains pressure, density, volume, and temperature of the main dataset discussed in the paper (10 and 100 GPa). Also included are the diffusivities of iron and hydrogen in units of m2/s, viscosity in units of Pa⋅s, average Fe-Fe and Fe-H coordination numbers and bond lengths, as well as the molecular hydrogen abundance and the average number of Fe in H1, H2, and H3 clusters. Nominal pressures, Pnom are provided as these data were generalized within the text; their actual pressure, Pavg, are provided as well. (v1 vs v2: viscosity columns ([visc_Pas, visc_std] were updated, as a typo was discovered in the calculation of viscosity and it was a factor of 1/3 too small; May 2024: added molecular hydrogen data; October 2024, viscosity updated to include a neglected factor of 1/2).</p> <p>ds02.xlsx</p> <p>Contains all the data used in fitting the equation of state (v1-2 vs May 2024: P<10 GPa added to equation of state fit). The first sheet includes the molar volume, temperature, pressure (P), the magnetism corrected pressure (P_magcor115), and the residuals from the equation of state fits (both Birch Murnaghan and Vinet). The second sheet includes the comparison of spin polarized and non-spin polarized pressure in the iron hydrides at ~1 GPa. The third sheet includes the comparison of spin polarized and non-spin polarized pressure in pure iron. </p> <p>FeH-EOS_XfromrhoPT.py</p> <p>added in Oct 2024 update, a simple python function that estimates the hydrogen content of an Fe-H melt with a given density, pressure, and temperature </p>
Discovery of a Seven-Coordinated High Pressure CrSb2 Phase: Experimental Equation of State of TMSb2 (TM = Cr, Fe, Ru, Os)
<p>DFT calculations from: Discovery of a Seven-Coordinated High Pressure CrSb2 Phase: Experimental Equation of State of TMSb2 (TM = Cr, Fe, Ru, Os); Emma Ehrenreich-Petersen, Mads F. Hansen, Justin Jeanneau, Davide Ceresoli, Francesca Menescardi, Martin Ottesen, Vitali Prakapenka, Sergey N. Tkachev and Martin Bremholm; submitted to Inorg. Chem. (2023)</p>
Equation of State of Liquid Fe7C3 and Thermodynamic Modeling of the Liquidus Phase Relations in the Fe-C System
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Thermal Equations of State of Corundum and Rh2O3 (II)-type Al2O3 up to 153 GPa and 3400 K
<p>Supporting information for the article "<strong>Thermal Equations of State of Corundum and Rh<sub>2</sub>O<sub>3</sub> (II)-type Al<sub>2</sub>O<sub>3</sub></strong> <strong>up to 153 GPa and 3400 K</strong>"</p>
Compressibility and the equation of state of an optical quantum gas in a box
<p>This repository contains the data presented in the manuscript titled "Compressibility and the equation of state of an optical quantum gas in a box" by E. Busley et al., Science 375, 1403–1406 (2022), arXiv:2112.12787.</p> <p>1) The files named 'Fig{1,2,3,4}_raw.xlsx' contain the final data sets relevant to reproduce all plots shown in the paper</p> <p>2) The zipped folder 'raw_scripts' contains Mathematica and Python scripts as well as the relevant raw data, which allow the reproduction of the data shown in the paper</p>
Data file needed for implementation of the Helmholtz equation of state in the Phantom smoothed particle hydrodynamics and magnetohydrodynamics code
<p>** this file is downloaded automatically on running Phantom **<br><br>This is a datafile containing information needed to utilise the Helmholtz equation of state (<a href="http://adsabs.harvard.edu/abs/2000ApJS..126..501T">Timmes & Swesty 2000</a>) implemented in the Phantom smoothed particle hydrodynamics and magnetohydrodynamics code (<a href="http://adsabs.harvard.edu/abs/2018PASA...35...31P">Price et al. 2018</a>). </p> <p>Primarily used to model degenerate matter in white dwarfs</p> <p>For information about how to read the file and its contents, refer to the relevant module in the phantom source code (<a href="https://github.com/danieljprice/phantom/blob/master/src/main/eos_helmholtz.f90">eos_helmholtz.f90</a>)</p>
Optimal neutron-star mass ranges to constrain the equation of state of nuclear matter with electromagnetic and gravitational-wave observations: Animated Fig. 1
<p>This repository includes the animated version of Fig. 1 in https://arxiv.org/abs/1905.04900.</p>
Models and data for: State estimation of a physical system without governing equations
<p>Contains the accompanying data and models for the paper State estimation of a physical system with unknown governing equations. Accompanying code can be found here: https://github.com/coursekevin/svise</p> <p> </p>
Data supplement for "Localized states in the conserved Swift-Hohenberg equation with cubic nonlinearity [Phys. Rev. E 87, 042915 (2013)]"
<p>Data sets and user-defined files for continuation tool auto07p for most figures of the paper "Localized states in the conserved Swift-Hohenberg equation with cubic nonlinearity" [<em>Phys. Rev. E </em> <strong>87</strong>, 042915 (2013)] with abstract "The conserved Swift-Hohenberg equation with cubic nonlinearity provides the simplest microscopic description of the thermodynamic transition from a fluid state to a crystalline state. The resulting phase field crystal model describes a variety of spatially localized structures, in addition to different spatially extended periodic structures. The location of these structures in the temperature versus mean order parameter plane is determined using a combination of numerical continuation in one dimension and direct numerical simulation in two and three dimensions. Localized states are found in the region of thermodynamic coexistence between the homogeneous and structured phases, and may lie outside of the binodal for these states. The results are related to the phenomenon of slanted snaking but take the form of standard homoclinic snaking when the mean order parameter is plotted as a function of the chemical potential, and are expected to carry over to related models with a conserved order parameter."</p> <p> </p>
Bayesian modeling of the equation-of-state for liquid iron in Earth's outer core
<p>Input data of Matsumura et al.</p>
GP ensemble of neutron star equations of state
<p>GP ensemble of neutron star equations of state used in arXiv:2303.11356</p>
Inner Core Composition of the Moon and Ganymede revealed by Thermal Equation of State of Fe0.99C0.01 alloy
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