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13 results for “Smoothed particle hydrodynamics”
Binary data file needed for the Shen et al. (2011) equation of state implemented in the Phantom smoothed particle hydrodynamics and magnetohydrodynamics code
<p>** this file is downloaded automatically from this repository on running Phantom **</p> <p>Contains information needed to load the <a href="http://adsabs.harvard.edu/abs/2011PhRvC..83c5802S">Shen, Horowitz & Teige (2011)</a> equation of state for nuclear matter in Phantom simulations</p> <p>The data file is a binary data file that enables a fast read of the information listed in the ascii tables given in the supplementary material of the Shen et al paper. The original ascii data files can be found here:</p> <p><a href="https://journals.aps.org/prc/supplemental/10.1103/PhysRevC.83.035802">https://journals.aps.org/prc/supplemental/10.1103/PhysRevC.83.035802</a></p> <p>For information on how to read this file, see the Phantom source code (<a href="https://github.com/danieljprice/phantom/blob/master/src/main/eos_shen.f90">eos_shen.f90</a>)</p>
Turbulence pattern files used for star cluster formation in the Phantom smoothed particle hydrodynamics and magnetohydrodynamics code
<p>** these files are automatically downloaded by Phantom on running the code **</p> <p>The files here are sample cubes containing turbulent driving patterns for the velocity field (vx, vy and vz) used to initiate star cluster formation simulations in the Phantom smoothed particle hydrodynamics and magnetohydrodynamics code</p> <p>These can be used to set up initial conditions for a set of simulations similar to those shown in <a href="http://adsabs.harvard.edu/abs/2003MNRAS.339..577B">Bate, Bonnell & Bromm (2003)</a>. The files here are not the original driving patterns used in the BBB03 simulations, but have the same structure, and give a default driving pattern that can be used without having to re-generate the files. A similar set of files was used for the simulations published in <a href="https://ui.adsabs.harvard.edu/abs/2017MNRAS.465..105L">Liptai et al. (2017)</a>.</p> <p>The files were generated with a piece of code written by Volker Bromm, which was originally part of Matthew Bate's sphNG simulation code.</p> <p>For details of how to read these files, see the Phantom source code (<a href="https://github.com/danieljprice/phantom/blob/master/src/setup/velfield_fromcubes.f90">src/setup/velfield_fromcubes.f90</a>)</p>
Data files for the tabulated MESA equation of state in the Phantom smoothed particle hydrodynamics and magnetohydrodynamics code
<div> <div> <div> <p>** These tables are automatically downloaded from this repository when running phantom **<br><br>This tabulated equation of state in PHANTOM is adapted from the logPgas − Temperature equation of state tables provided with the open source package Modules for Experiments in Stellar Astrophysics MESA (Paxton et al. 2011). Details of the data, originally compiled from blends of equations of state from Saumon, Chabrier, & van Horn (1995) (SCVH), Timmes & Swesty (2000), Rogers & Nayfonov (2002, also the 2005 update), Potekhin & Chabrier (2010) and for an ideal gas, are outlined by Paxton et al. (2011).</p> <p>Code to read these tables is available as part of phantom (<a href="https://github.com/danieljprice/phantom/blob/master/src/main/eos_mesa_microphysics.f90">src/main/eos_mesa.f90</a>). The original version of these tables and the module to read them was contributed by Tom Constantino from the MUSIC code (<a href="https://ui.adsabs.harvard.edu/abs/2017A&A...600A...7Ga">Goffrey et al. 2017</a>), and the phantom implementation described in <a href="http://adsabs.harvard.edu/abs/2018PASA...35...31P">Price et al. (2018)</a>.The current tables were created by Tom Reichardt for the paper Reichardt et al. (2020):<br><br><a href="https://ui.adsabs.harvard.edu/abs/2020MNRAS.494.5333R/abstract">https://ui.adsabs.harvard.edu/abs/2020MNRAS.494.5333R/abstract</a></p> </div> </div> </div> <p>Figure 1 in Reichardt et al. (2020) shows the pressure, temperature, Gamma and P/Pideal shown as a function of internal energy and density from these tables</p>
Data file needed for star cluster setup in Phantom smoothed particle hydrodynamics and magnetohydrodynamics code
<p>** this file is automatically downloaded by Phantom when running the starcluster setup **</p> <p>This is a small ascii file containing positions and velocities of stars utilised in the "starcluster" configuration in the Phantom smoothed particle hydrodynamics and magnetohydrodynamics code (<a href="http://adsabs.harvard.edu/abs/2018PASA...35...31P">Price et al. 2018</a>). It is used to set up a collection of N-body particles.</p> <p>The star cluster setup (and the data file) were written by Yann Bernard as part of his PhD thesis at<strong> </strong>Université Grenoble Alpes. The datafile is published here so it can be used in the automated code testing via github actions. </p> <p>The columns are mass, position (x,y,z) and velocity (vx,vy,vz) for all of the stars in the simulation</p>
Binary data file used for analysis_common_envelope unit testing in the Phantom smoothed particle hydrodynamics and magnetohydrodynamics code
<p>** this file is automatically downloaded as part of the Phantom github actions tests **</p> <p>This is an example snapshot from a Phantom simulation of a common envelope interaction, taken from the paper by <a href="https://ui.adsabs.harvard.edu/abs/2022MNRAS.517.3181G">González-Bolívar et al. (2022)</a>. It is posted here primarily in order to perform unit and regression testing on the <a href="https://github.com/danieljprice/phantom/blob/master/src/utils/analysis_common_envelope.f90">analysis_common_envelope</a> module 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>
Simulating Wave Characteristics with Second-Order Wave Generator using Smoothed Particle Hydrodynamics (SPH)
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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>
Data for 'Adaptive Particle Refinement for compressible Smoothed Particle Hydrodynamics'
<p>Contains necessary files to recreate the simulations presented in Adaptive Particle Refinement for compressible Smoothed Particle Hydrodynamics (under review). We have also included the files to recreate the rendered plots presented in the paper. There are seven folders;</p> <ol> <li>Circumbinary disc test</li> <li>Planet-disc test</li> <li>Flyby test</li> <li>Periodic box tests</li> <li>Firehose test</li> <li>Nchild test</li> <li>Kernel test with planet disc interaction</li> </ol> <p>Within each of these folders there are sub-folders that refer to each specific simulation presented in the paper. Each folder contains the necessary .setup and .in file as well as the .ev files where applicable. Where rendered figures have been made, the corresponding dump files are also included here. All figures were made using sarracen (https://github.com/ttricco/sarracen/).</p>
Appendices A-B-C for Malfait et al. 2024(a), Impact of HI cooling and study of accretion disks in AGB wind-companion smoothed particle hydrodynamic simulations
<p>Appendices A, B, C with figures, of the paper Malfait et al. 2024(a) "Impact of HI cooling and study of accretion disks in AGB wind-companion smoothed particle hydrodynamic simulations".</p>
Data of smoothed particle hydrodynamic giant impact simulations for the paper "A super-massive Neptune-sized planet"
<p>This dataset contains data from the article:</p> <p>L. Naponiello et al. 2023 "A super-massive Neptune-sized planet". DOI: https://doi.org/10.1038/s41586-023-06499-2</p> <p>The dataset comprises initial conditions and final snapshots of the smoothed particle hydrodynamics simulations selected in the paper.</p> <p>All the simulations were performed using <a href="https://swift.com">SWIFT</a> with initial condtions generated using <a href="https://github.com/srbonilla/WoMa">WoMa</a>. The planets are modeled with forsterite core (see <a href="https://github.com/ststewart/aneos-forsterite-2019">Link</a>), water middle layer (see <a href="https://ui.adsabs.harvard.edu/abs/2020A%26A...643A.105H/abstract">link</a>), and H&He mixture atmosphere top layer (see <a href="https://ui.adsabs.harvard.edu/abs/1980JGR....85..225H/abstract">link</a>).</p> <p>We simulated three different pre-impact compositions: water-rich by mass (22.5 % rock, 67.5 % water, 10 % H/He), equal rock and water (45 % rock, 45 % water, 10 % H/He), and rock-rich (67.5 % rock, 22.5 % water, 10 % H/He). These are located in the "data.zip" file under the folders "water rich", "equal_water_rock", and "rock_rich", respectively. In each simulation subfolder, "snapshot_0000.hdf5" is the initial condition file, where the target and impactor are separated by a distance that allows contact to occur 1 hour after the start of the simulation. "snapshot_00xx.hdf5" is the final snapshot of that simulation, where "xx" is the simulation time in hours. For example, "snapshot_0015.hdf5" is the snapshot taken after 15 hours of the simulation.</p>
Initial conditions for galaxy merger setup in the Phantom smoothed particle hydrodynamics and magnetohydrodynamics code
<p>** these files are downloaded automatically by Phantom when running the code **</p> <p>The two files here contain initial conditions (particle positions, velocities etc) for the sample galaxy merger simulation shown in Figure 55 of the Phantom code paper (<a href="http://adsabs.harvard.edu/abs/2018PASA...35...31P">Price et al. 2018</a>). They were created by James Wurster as part of a code comparison with the Hydra code described in section 6.4 of the paper.</p> <p>The files were originally created for use in <a href="http://adsabs.harvard.edu/abs/2013MNRAS.431..539W">Wurster & Thacker (2013)</a></p> <p>For details of how to read these files, see the Phantom source code (<a href="https://github.com/danieljprice/phantom/blob/master/src/setup/setup_galaxies.f90">setup_galaxies.f90</a>)</p>
Data file for turbulence driving pattern in the Phantom smoothed particle hydrodynamics and magnetohydrodynamics code
<p>** this file is automatically downloaded by phantom on running the code **</p> <p>This is the default driving pattern file used in the "turbdrive" setup of the Phantom smoothed particle hydrodynamics and magnetohydrodynamics code, which was originally written for the set of simulations shown in <a href="http://adsabs.harvard.edu/abs/2010MNRAS.406.1659P">Price & Federrath (2010)</a>. The driving pattern file was originally created by Christoph Federrath.</p> <p>For details and references on the Ornstein-Uhlenbeck stochastic turbulent driving algorithm itself, see section 2.5 of the Phantom code paper (<a href="http://adsabs.harvard.edu/abs/2018PASA...35...31P">Price et al. 2018</a>).</p> <p>The same pattern file has been used in several subsequent studies, including <a href="http://adsabs.harvard.edu/abs/2016MNRAS.461.1260T">Tricco, Price & Federrath (2016)</a> and <a href="http://adsabs.harvard.edu/abs/2017MNRAS.471L..52T">Tricco, Price & Laibe (2017)</a>.</p> <p>For details on how to read this file see the Phantom source code (<a href="https://github.com/danieljprice/phantom/blob/master/src/main/forcing.F90">src/main/forcing.f90</a>)</p>
Data for "Impact of HI cooling and study of accretion disks in AGB wind-companion smoothed particle hydrodynamic simulations"
<p>Additional material to Malfait et al. 2024(a) "Impact of HI cooling and study of accretion disks in AGB wind-companion smoothed particle hydrodynamic simulations"</p> <p>This contains input files and final output dumps of the Phantom simulations of this paper, and some movies to illustrate the complex flows within the binary systems.</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> <p> </p>
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