Hybrid Adaptive Ray-Moment Method (HARM): A Highly Parallel Method for Radiation Hydrodynamics on Adaptive Grids
arXiv:1607.01802 · doi:10.1016/j.jcp.2016.10.048
Abstract
We present a highly-parallel multi-frequency hybrid radiation hydrodynamics algorithm that combines a spatially-adaptive long characteristics method for the radiation field from point sources with a moment method that handles the diffuse radiation field produced by a volume-filling fluid. Our Hybrid Adaptive Ray-Moment Method (HARM) operates on patch-based adaptive grids, is compatible with asynchronous time stepping, and works with any moment method. In comparison to previous long characteristics methods, we have greatly improved the parallel performance of the adaptive long-characteristics method by developing a new completely asynchronous and non-blocking communication algorithm. As a result of this improvement, our implementation achieves near-perfect scaling up to processors on distributed memory machines. We present a series of tests to demonstrate the accuracy and performance of the method.
27 pages, 8 figures, submitted to Journal of Computational Physics. Referee comments received and will be addressed in final version
References in corpus (7)
- Athena: A New Code for Astrophysical MHD
- The Dynamics of Radiation Pressure-Dominated HII Regions
- A scheme for radiation pressure and photon diffusion with the M1 closure in RAMSES-RT
- Equations and Algorithms for Mixed Frame Flux-Limited Diffusion Radiation Hydrodynamics
- Magnetohydronamic Evolution of HII Regions in Molecular Clouds: Simulation Methodology, Tests, and Uniform Media
- An Unstable Truth: How Massive Stars get their Mass
- A general hybrid radiation transport scheme for star formation simulations on an adaptive grid
Cited by in corpus (13)
- The dynamics and outcome of star formation with jets, radiation, winds, and supernovae in concert
- An Unstable Truth: How Massive Stars get their Mass
- Forming spectroscopic massive proto-binaries by disk fragmentation
- Zooming in on Individual Star Formation: Low- and High-mass Stars
- The Role of Outflows, Radiation Pressure, and Magnetic Fields in Massive Star Formation
- Modeling UV Radiation Feedback from Massive Stars: I. Implementation of Adaptive Ray Tracing Method and Tests
- The Astrochemical Impact of Cosmic Rays in Protoclusters I: Molecular Cloud Chemistry
- Collapse of turbulent massive cores with ambipolar diffusion and hybrid radiative transfer I. Accretion and multiplicity
- Tree-based solvers for adaptive mesh refinement code FLASH -- II: radiation transport module TreeRay
- VETTAM: A scheme for radiation hydrodynamics with adaptive mesh refinement using the variable Eddington tensor method
- Radiation transport methods in star formation simulations
- PION: Simulating bow shocks and circumstellar nebulae
- Numerical Methods for Simulating Star Formation