Moving and Reactive Boundary Conditions in Moving-Mesh Hydrodynamics
arXiv:2002.04287 · doi:10.1093/mnras/staa1031
Abstract
We outline the methodology of implementing moving boundary conditions into the moving-mesh code MANGA. The motion of our boundaries is reactive to hydrodynamic and gravitational forces. We discuss the hydrodynamics of a moving boundary as well as the modifications to our hydrodynamic and gravity solvers. Appropriate initial conditions to accurately produce a boundary of arbitrary shape are also discussed. Our code is applied to several test cases, including a Sod shock tube, a Sedov-Taylor blast wave and a supersonic wind on a sphere. We show the convergence of conserved quantities in our simulations. We demonstrate the use of moving boundaries in astrophysical settings by simulating a common envelope phase in a binary system, in which the companion object is modeled by a spherical boundary. We conclude that our methodology is suitable to simulate astrophysical systems using moving and reactive boundary conditions.
arXiv comment12 pages, 8 figures, submitted to MNRAS
References in corpus (31)
- Modules for Experiments in Stellar Astrophysics (MESA)
- Modules for Experiments in Stellar Astrophysics (MESA): Giant Planets, Oscillations, Rotation, and Massive Stars
- Modules for Experiments in Stellar Astrophysics (MESA): Binaries, Pulsations, and Explosions
- E pur si muove: Galiliean-invariant cosmological hydrodynamical simulations on a moving mesh
- Introducing the Illustris Project: Simulating the coevolution of dark and visible matter in the Universe
- Modules for Experiments in Stellar Astrophysics (MESA): Convective Boundaries, Element Diffusion, and Massive Star Explosions
- Modules for Experiments in Stellar Astrophysics (MESA): Pulsating Variable Stars, Rotation, Convective Boundaries, and Energy Conservation
- A Multi-Code Analysis Toolkit for Astrophysical Simulation Data
- Common Envelope Evolution: Where we stand and how we can move forward
- The first gravitational-wave source from the isolated evolution of two 40-100 Msun stars
- Gasoline: An adaptable implementation of TreeSPH
- An AMR Study of the Common Envelope Phase of Binary Evolution
- Simulating the Common Envelope Phase of a Red Giant Using SPH and Uniform Grid Codes
- A Necessary Condition for Individual Time-Steps in SPH Simulations
- Hydrodynamic moving-mesh simulations of the common envelope phase in binary stellar systems
- TESS: A Relativistic Hydrodynamics Code on a Moving Voronoi Mesh
- Recombination energy in double white dwarf formation
- A Validated Nonlinear Kelvin-Helmholtz Benchmark for Numerical Hydrodynamics
- Hydrodynamical moving-mesh simulations of the tidal disruption of stars by supermassive black holes
- Common Envelope Evolution on a Moving Mesh
- Magnetized Moving Mesh Merger of a Carbon-Oxygen White Dwarf Binary
- Common Envelope Wind Tunnel: The Effects of Binary Mass Ratio and Implications for the Accretion-Driven Growth of LIGO Binary Black Holes
- An ALE-type discrete unified gas kinetic scheme for low-speed continuum and rarefied flow simulations with moving boundaries
- A 3D radiation-hydrodynamic AGB binary model
- Super-Eddington accretion of dusty gas onto seed black holes: metallicity-dependent efficiency of mass growth
- How Drag Force Evolves in Global Common Envelope Simulations
- Energy Budget and Core-Envelope Motion in Common Envelope Evolution
- A Moving Mesh Hydrodynamic Solver for ChaNGa
- Time Dependent Radiation Hydrodynamics on a Moving Mesh
- Grid Noise in Moving Mesh Codes: Fixing The Volume Inconsistency Problem
- A parallel dynamic overset grid framework for immersed boundary methods