Data from: "Eddington envelopes: The fate of stars on parabolic orbits tidally disrupted by supermassive black holes" (Price et al. 2024)

<p>The paper by Price et al. (2024; <a href="https://arxiv.org/abs/2404.09381">arXiv:2404.09381</a>) simulates the tidal disruption of a one solar mass polytropic star by a million-solar-mass supermassive black hole, using the Phantom general relativistic smoothed particle hydrodynamics code (Price et al. 2018). The code used to perform the simulations is available at:</p> <p><a href="https://github.com/danieljprice/phantom">https://github.com/danieljprice/phantom</a></p> <p>This dataset contains:</p> <ol> <li>Scripts, intermediate data products and other small files used to create each figure in the paper</li> <li>Selected snapshots and other raw data from the four main calculations shown in the paper</li> </ol> <p>The main datasets contain parameter files and snapshots from the simulations used to create figures in the paper.small data files from the simulations and post-processing scripts used to create the scientific results and figures shown in the paper. Each simulation dataset contains:</p> <p><strong>.setup file:</strong> parameter file used by phantomsetup to create the initial conditions for the star itself<br><br><strong>.in file:</strong> parameter file used by phantom to perform the calculation<br><br><strong>tde_00000, tde_00100, tde_00200 etc:</strong> binary code snapshots containing raw data (particle positions, velocities, thermal energy, etc), these can be read/visualised/converted using the free and open source codes SPLASH (Price et al. 2007):<br><br><a href="https://github.com/danieljprice/splash">https://github.com/danieljprice/splash</a></p> <p>or Sarracen:</p> <p><a href="https://github.com/ttricco/sarracen">https://github.com/ttricco/sarracen</a></p> <p>SPLASH was used to create figures in the paper. The format and ways to read these data files are described in:</p> <p><a href="https://phantomsph.readthedocs.io/en/latest/user-guide/dumpfile.html">https://phantomsph.readthedocs.io/en/latest/user-guide/dumpfile.html</a></p> <p><strong>tde01.ev, tde02.ev etc:</strong> ascii files (see header) containing global quantities like total angular momentum, total momentum, total energy etc as a function of time. Each number corresponds to a restart of the code (i.e. resubmission of the job to the queue on the cluster).</p> <p><strong>tde01.log, tde02.log: </strong>output log from the simulations themselves, this contains some useful information like the unit scalings, typical timestep and code performance, hardware information etc.</p> <p><em><strong>.defaults, .limits, .units and .filenames:</strong> parameter files used by SPLASH to create particular figures. For example, to use the files lightcurve.defaults, lightcurve.units, lightcurve.limits and lightcurve.filenames one would plot using splash -p lightcurve</em></p> <p>The relevant raw data directories are:</p> <p><strong>beta1_hres: </strong>raw data from the adiabatic, beta=1 calculation</p> <p><strong>beta5_hres:</strong> raw data from the adiabatic, beta=5 calculation</p> <p><strong>beta1_isentropic: </strong>raw data from the isentropic, beta=1 calculation with a non-spinning black hole</p> <p><strong>beta1_isentropic_kerr_a99_i60:</strong> raw data from the isentropic, beta=1 calculation with a maximally-spinning black hole with the initial stellar orbit at an incliation of 60 degrees to the black hole spin</p> <p><strong>The procedure to recreate each figure and post-processing analysis used in the paper is explained in the README.md placed in each directory unpacked from the figureX.zip file</strong></p> <p>&nbsp;</p>