The paper by Price et al. (2024; arXiv:2404.09381) 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: https://github.com/danieljprice/phantom This dataset contains: Scripts, intermediate data products and other small files used to create each figure in the paper Selected snapshots and other raw data from the four main calculations shown in the paper 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: .setup file: parameter file used by phantomsetup to create the initial conditions for the star itself.in file: parameter file used by phantom to perform the calculationtde_00000, tde_00100, tde_00200 etc: 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):https://github.com/danieljprice/splash or Sarracen: https://github.com/ttricco/sarracen SPLASH was used to create figures in the paper. The format and ways to read these data files are described in: https://phantomsph.readthedocs.io/en/latest/user-guide/dumpfile.html tde01.ev, tde02.ev etc: 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). tde01.log, tde02.log: output log from the simulations themselves, this contains some useful information like the unit scalings, typical timestep and code performance, hardware information etc. .defaults, .limits, .units and .filenames: 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 The relevant raw data directories are: beta1_hres: raw data from the adiabatic, beta=1 calculation beta5_hres: raw data from the adiabatic, beta=5 calculation beta1_isentropic: raw data from the isentropic, beta=1 calculation with a non-spinning black hole beta1_isentropic_kerr_a99_i60: 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 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