1702.03930.pdf (14.91 MB)
PHANTOM: A Smoothed Particle Hydrodynamics and Magnetohydrodynamics Code for Astrophysics
journal contributionposted on 2019-03-25, 11:56 authored by DJ Price, J Wurster, TS Tricco, C Nixon, S Toupin, A Pettitt, C Chan, D Mentiplay, G Laibe, S Glover, C Dobbs, R Nealon, D Liptai, H Worpel, C Bonnerot, G Dipierro, G Ballabio, E Ragusa, C Federrath, R Iaconi, T Reichardt, D Forgan, M Hutchison, T Constantino, B Ayliffe, K Hirsh, G Lodato
We present Phantom, a fast, parallel, modular, and low-memory smoothed particle hydrodynamics and magnetohydrodynamics code developed over the last decade for astrophysical applications in three dimensions. The code has been developed with a focus on stellar, galactic, planetary, and high energy astrophysics, and has already been used widely for studies of accretion discs and turbulence, from the birth of planets to how black holes accrete. Here we describe and test the core algorithms as well as modules for magnetohydrodynamics, self-gravity, sink particles, dust–gas mixtures, H2 chemistry, physical viscosity, external forces including numerous galactic potentials, Lense–Thirring precession, Poynting–Robertson drag, and stochastic turbulent driving. Phantom is hereby made publicly available.
PHANTOM is the result of interactions over the years with numerous talented and interesting people. Particular mentions go to Joe Monaghan, Matthew Bate, and Stephan Rosswog from whom I (DP) learnt and discussed a great deal about SPH over the years. We also thank Walter Dehnen, James Wadsley, Evghenii Gaburov, Matthieu Viallet, and Pedro Gonnet for stimulating interactions. This work and the public release of PHANTOM was made possible by the award of a four-year Future Fellowship (FT130100034) to DJP from the Australian Research Council (ARC), as well as funding via Discovery Projects DP130102078 (funding James Wurster and Mark Hutchison) and DP1094585 (which funded Guillaume Laibe and partially funded Terrence Tricco). CN is supported by the Science and Technology Facilities Council (grant number ST/M005917/1). CF gratefully acknowledges funding provided by ARC Discovery Projects (grants DP150104329 and DP170100603). SCOG acknowledges support from the Deutsche Forschungsgemeinschaft via SFB 881 (sub-projects B1, B2, B8) and from the European Research Council via the ERC Advanced Grant ‘STARLIGHT’ (project number 339177). This work was supported by resources awarded under Astronomy Australia Ltd’s merit allocation scheme on the gSTAR and swinSTAR national facilities at Swinburne University of Technology and the Pawsey National Supercomputing Centre. gSTAR and swinSTAR are funded by Swinburne and the Australian Government’s Education Investment Fund. We thank Charlene Yang from the Pawsey Supercomputing Centre for particular help and assistance as part of a Pawsey uptake project. We used SPLASH for many of the figures (Price 2007). We thank Max Tegmark for his excellent icosahedron module used in various analysis routines.
CitationPublications of the Astronomical Society of Australia, 2018, 35, e031, 82 pages
Author affiliation/Organisation/COLLEGE OF SCIENCE AND ENGINEERING/Department of Physics and Astronomy
- AM (Accepted Manuscript)
Published inPublications of the Astronomical Society of Australia
PublisherCambridge University Press (CUP) for Astronomical Society of Australia
NotesThe file associated with this record is under embargo until 6 months after publication, in accordance with the publisher's self-archiving policy. The full text may be available through the publisher links provided above.
Science & TechnologyPhysical SciencesAstronomy & Astrophysicsaccretion, accretion diskshydrodynamicsISM: generalmagnetohydrodynamics (MHD)methods: numericalINITIAL MASS FUNCTIONBINARY STAR-FORMATIONMAGNETIC GAS CLOUDSN-BODY SIMULATIONSEQUATION-OF-STATE3-DIMENSIONAL NUMERICAL SIMULATIONSLIMITED DIFFUSION-APPROXIMATIONGALAXY CLUSTER SIMULATIONSTIDAL DISRUPTION EVENTSSELF-GRAVITATING DISCS