Gasoline: An adaptable implementation of TreeSPH

Abstract

The key algorithms and features of the Gasoline code for parallel hydrodynamics with self-gravity are described. Gasoline is an extension of the efficient Pkdgrav parallel N-body code using smoothed particle hydrodynamics. Accuracy measurements, performance analysis and tests of the code are presented. Recent successful Gasoline applications are summarized. These cover a diverse set of areas in astrophysics including galaxy clusters, galaxy formation and gas-giant planets. Future directions for gasdynamical simulations in astrophysics and code development strategies for tackling cutting edge problems are discussed.

30 pages, 11 figures, submitted to New Astronomy. Movies and high resolution images are available at http://imp.mcmaster.ca/images

References in corpus (1)

• Formation of giant planets by fragmentation of protoplanetary disks

Cited by in corpus (507)

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• The secular growth of bars revealed by flat (peak + shoulders) density profiles
• One-Two Quench: A Double Minor Merger Scenario
• The Adaptive TreePM: An Adaptive Resolution Code for Cosmological N-body Simulations
• The EOS/Resolution Conspiracy: Convergence in Proto-Planetary Collision Simulations
• A minor merger scenario for the ultraluminous X-ray source ESO 243-49 HLX-1 - II. Constraints from photometry
• Theory of Stellar Population Synthesis with an application to N-Body simulations
• Explaining the chemical trajectories of accreted and in-situ halo stars of the Milky Way
• Multiple regimes and coalescence timescales for massive black hole pairs ; the critical role of galaxy formation physics
• Testable predictions of outside-in age gradients in dwarf galaxies of all types
• Could Uranus and Neptune form by collisions of planetary embryos?
• Star cluster formation and feedback in different environments of a Milky Way-like galaxy
• Particle tagging and its implications for stellar population dynamics
• The Properties of Bound and Unbound Molecular Cloud Populations Formed in Galactic Disc Simulations
• Direct detection of precursors of gas giants formed by gravitational instability with the Atacama Large Millimetre/sub-millimetre Array
• The luminosity function of diverse satellite galaxy systems
• Connecting the Dots: Analyzing Synthetic Observations of Star-Forming Clumps in Molecular Clouds
• The role of gravitational recoil in the assembly of massive black hole seeds
• Differences in star formation activity between tidally triggered and isolated bars: a case study of NGC 4303 and NGC 3627
• Measuring Galactic Dark Matter through Unsupervised Machine Learning
• Analytic and numerical realisations of a disk galaxy
• Generation of gravitational waves and tidal disruptions in clumpy galaxies
• The relative efficiencies of bars and clumps in driving disc stars to retrograde motion
• Predicted Stellar Kinematics of a Kiloparsec-Scale Nuclear Disc (or Ring) in the Milky Way
• The complete census of molecular hydrogen in a simulated disc galaxy
• TREVR: A general $Nlo{g}^{2}N$ radiative transfer algorithm
• The temperature of hot gas in galaxies and clusters: baryons dancing to the tune of dark matter
• Chemical Abundance Patterns and the Early Environment of Dwarf Galaxies
• Gas Accretion and Angular Momentum
• Hierarchical generative models for star clusters from hydro-dynamical simulations
• Self-Interacting Dark Matter and the Delay of Super-Massive Black Hole Growth
• FORECAST: a flexible software to forward model cosmological hydrodynamical simulations mimicking real observations
• Is the vast polar structure of dwarf galaxies a serious problem for lambda cold dark matter?
• The influence of dense gas rings on the dynamics of a stellar disk in the Galactic center
• A high fidelity Milky Way simulation with Kraken, Gaia-Enceladus, and Sequoia analogues: clues to their accretion histories
• SPH to Grid: a new integral conserving method
• The impact of binaries on the evolution of star clusters from turbulent molecular clouds
• Proto-Brown Dwarf Disks as Products of Protostellar Disk Encounters
• The pattern speeds of vertical breathing waves
• Smoothed-Particle Hydrodynamics Models: Implementation Features on GPUs
• Gas stripping and mixing in galaxy clusters: A numerical comparison study
• CLUES about M33: the reversed radial stellar age gradient in the outskirts of Triangulum galaxy
• Numerical simulations of bar formation in the Local Group
• Exploring the Evolution of Massive Clumps in Simulations that Reproduce the Observed Milky Way α-element Abundance Bimodality
• Terapixel imaging of cosmological simulations
• Angular momentum evolution of bulge stars in disc galaxies in NIHAO
• Implementing and comparing sink particles in AMR and SPH
• PHoToNs--A Parallel Heterogeneous & Threads oriented code for cosmological N-body simulation
• Massive Black Hole Recoil in High Resolution Hosts
• The origin of type-I profiles in cluster lenticulars: An interplay between ram pressure stripping and tidally-induced spiral migration
• Testing core creation in hydrodynamical simulations using the HI kinematics of field dwarfs
• The Anatomy of a Star-Forming Galaxy II: the role of FUV heating via dust
• Consequences of cosmic microwave background-regulated star formation
• Origin and Evolution of Structure and Nucleosynthesis for Galaxies in the Local Group
• Mesh-free hydrodynamics in PKDGRAV3 for galaxy formation simulations
• The tilting rate of the Milky Way's disc
• A Modified TreePM Code
• A disrupted bulgeless satellite galaxy as counterpart of the ultraluminous X-ray source ESO 243-49 HLX-1
• Unbound Star-forming Molecular Clouds
• Addressing via N-body simulations the distribution of the satellite tidal debris in the Milky Way environment
• A scaling relation for core heating by giant impacts and implications for dynamo onset
• Implementing Dust Shielding as a Criteria for Star Formation
• Astrophysical Particle Simulations on Heterogeneous CPU-GPU Systems
• A Tale of Two Clump Masses: A New Way to Study Clump Formation in Simulations
• Numerical dependencies of the galactic dynamo in isolated galaxies with SPH
• Self-similar galaxy dynamics below the de Sitter scale of acceleration
• The Radial Distribution of Mono-Metallicity Populations in the Galactic Disk as Evidence for Two-Phase Disk Formation
• The Pressure of the Star Forming ISM in Cosmological Simulations
• Moving and Reactive Boundary Conditions in Moving-Mesh Hydrodynamics
• Haloes at the ragged edge: The importance of the splashback radius
• A Systematic Survey of Moon-Forming Giant Impacts. II. Rotating bodies
• GalaxyFlow: Upsampling Hydrodynamical Simulations for Realistic Mock Stellar Catalogs
• Accelerating self-gravitating hydrodynamics simulations with adaptive force updates
• The HI Structure of the Local Volume Dwarf Galaxy Pisces A
• High accuracy power spectra including baryonic physics in dynamical Dark Energy models
• A MARVEL-ous study of how well galaxy shapes reflect Dark Matter halo shapes in Cold Dark Matter Simulations
• Predictions for Detecting a Turndown in the Baryonic Tully Fisher Relation
• Predicted Trends in Milky Way Bulge Proper Motion Rotation Curves: future Prospects for HST and LSST
• How stars formed in warps settle into (and contaminate) thick discs
• Visualizing Astrophysical N-body Systems
• Astrophysics with the Laser Interferometer Space Antenna
• SWIFT: task-based hydrodynamics and gravity for cosmological simulations
• A self-gravity module for the PLUTO code
• Stellar Migration and Chemical Enrichment in the Milky Way Disc: A Hybrid Model
• NIHAO-RiNG: A Comparison of Simulated Disc Galaxies from GASOLINE and GIZMO
• Properties of loss cone stars in a cosmological galaxy merger remnant
• Multi-scale simulations of merging galaxies with supermassive black holes
• Survivors and Zombies: The Quenching and Disruption of Satellites around Milky Way Analogs
• SPH Methods in the Modelling of Compact Objects
• Quenching vs. Quiescence: forming realistic massive ellipticals with a simple starvation model
• Clues to the nature of dark matter from first galaxies
• Constraining the physical properties of gas in high-z galaxies with far-infrared and submillimetre line ratios
• Gaseous Dynamical Friction: a Numerical Study of Extended Perturbers
• The Impact of Baryons on the Large-Scale Structure of the Universe
• The COS-Holes Survey: Connecting Galaxy Black Hole Mass with the State of the CGM
• Diversity of dwarf galaxy IR-submm emission patterns: CLUES from hydrodynamical simulations
• Protoplanet collisions: new scaling laws from SPH simulations
• A theoretical investigation of far-infrared fine structure lines at $z>6$ and of the origin of the [OIII]88/[CII]158 enhancement
• The Chemical and Dynamical Evolution of Isolated Dwarf Galaxies
• Simulating gravitational motion, gas dynamics, and structure in the cosmos
• The chemical and spatial variations of the bulge's velocity ellipsoids
• The Formation of Dwarf Galaxy Disks
• High precision spectra at large redshift for dynamical DE cosmologies
• Properties of Carbon-Oxygen White Dwarf Merger Remnants
• The small-scale turbulent dynamo in smoothed particle magnetohydrodynamics
• Dust and gas modelling in radiative transfer simulations of disc-dominated galaxies with RADMC-3D
• Detectability of large-scale counter-rotating stellar disks in galaxies with integral-field spectroscopy
• DIAPHANE: a Portable Radiation Transport Library for Astrophysical Applications
• Size-scaling of clump instabilities in turbulent, feedback regulated disks
• Validating the CROCODILE model within the AGORA galaxy simulation framework
• Phase spirals induced by the gas warp
• Did Uranus' regular moons form via a rocky giant impactor?