A smooth particle hydrodynamics code to model collisions between solid, self-gravitating objects

Abstract

Modern graphics processing units (GPUs) lead to a major increase in the performance of the computation of astrophysical simulations. Owing to the different nature of GPU architecture compared to traditional central processing units (CPUs) such as x86 architecture, existing numerical codes cannot be easily migrated to run on GPU. Here, we present a new implementation of the numerical method smooth particle hydrodynamics (SPH) using CUDA and the first astrophysical application of the new code: the collision between Ceres-sized objects. The new code allows for a tremendous increase in speed of astrophysical simulations with SPH and self-gravity at low costs for new hardware. We have implemented the SPH equations to model gas, liquids and elastic, and plastic solid bodies and added a fragmentation model for brittle materials. Self-gravity may be optionally included in the simulations and is treated by the use of a Barnes-Hut tree. We find an impressive performance gain using NVIDIA consumer devices compared to our existing OpenMP code. The new code is freely available to the community upon request.

18 pages, 15 figures, accepted for publication in A&A

References in corpus (14)

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• A sparse octree gravitational N-body code that runs entirely on the GPU processor
• Numerical simulations of impacts involving porous bodies: I. Implementing sub-resolution porosity in a 3D SPH Hydrocode
• SPH calculations of asteroid disruptions: The role of pressure dependent failure models
• A Compound model for the origin of Earth's water
• Water/Icy Super-Earths: Giant Impacts and Maximum Water Content
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• Collisions between equal sized ice grain agglomerates
• SPH-based simulation of multi-material asteroid collisions
• Fragmentation of colliding planetesimals with water content

Cited by in corpus (29)

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• Origin of (2014) MU69-like Kuiper-belt contact binaries from wide binaries
• Realistic collisional water transport during terrestrial planet formation: Self-consistent modeling by an N-body--SPH hybrid code
• Binary orbital evolution driven by a circumbinary disc
• Triggering Sublimation-Driven Activity of Main Belt Comets
• Investigating the Feasibility of an Impact-Induced Martian Dichotomy
• Numerical Simulations of Regolith Sampling Processes
• Triggering the Activation of Main Belt Comets: The Effect of Porosity
• High Resolution Study of Planetesimal Formation by Gravitational Collapse of Pebble Clouds
• Impacts into rotating targets: angular momentum draining and efficient formation of synthetic families
• Collisional formation of massive exomoons of super-terrestrial exoplanets
• Moonfalls: Collisions between the Earth and its past moons
• Building Terrestrial Planets: Why results of perfect-merging simulations are not quantitatively reliable approximations to accurate modeling of terrestrial planet formation
• The influence of orbital resonances on the water transport to objects in the circumprimary habitable zone of binary star systems
• Protoplanet Collisions: Statistical Properties of Ejecta
• Residual Neural Networks for the Prediction of Planetary Collision Outcomes
• Selective Aggregation Experiments on Planetesimal Formation and Mercury-Like Planets
• Water delivery to dry protoplanets by hit-and-run collisions
• Metal-silicate mixing in planetesimal collisions
• Protoplanet collisions: new scaling laws from SPH simulations
• Modeling Solids in Nuclear Astrophysics with Smoothed Particle Hydrodynamics
• On the formation of terrestrial planets between two massive planets: The case of 55 Cancri
• The Formation of Habitable Planets in the Four-Planet System HD 141399
• Physical Analysis of Bennu Samples Reveals Regolith Production by Collisional Disruption on Near-Earth Asteroids
• Dust production through collisions between small bodies: an application to the G-ring arc
• The Material Point Method (MPM) for simulating hypervelocity impact on asteroids