Machine learning-driven conservative-to-primitive conversion in hybrid piecewise polytropic and tabulated equations of state
arXiv:2412.07836 · doi:10.3390/sym17091409
Abstract
We present a novel machine learning (ML) method to accelerate conservative-to-primitive inversion, focusing on hybrid piecewise polytropic and tabulated equations of state. Traditional root-finding techniques are computationally expensive, particularly for large-scale relativistic hydrodynamics simulations. To address this, we employ feedforward neural networks (NNC2PS and NNC2PL), trained in PyTorch and optimized for GPU inference using NVIDIA TensorRT, achieving significant speedups with minimal accuracy loss. The NNC2PS model achieves and errors of and , respectively, while the NNC2PL model exhibits even lower error values. TensorRT optimization with mixed-precision deployment substantially accelerates performance compared to traditional root-finding methods. Specifically, the mixed-precision TensorRT engine for NNC2PS achieves inference speeds approximately 400 times faster than a traditional single-threaded CPU implementation for a dataset size of 1,000,000 points. Ideal parallelization across an entire compute node in the Delta supercomputer (Dual AMD 64 core 2.45 GHz Milan processors; and 8 NVIDIA A100 GPUs with 40 GB HBM2 RAM and NVLink) predicts a 25-fold speedup for TensorRT over an optimally-parallelized numerical method when processing 8 million data points. Moreover, the ML method exhibits sub-linear scaling with increasing dataset sizes. We release the scientific software developed, enabling further validation and extension of our findings. This work underscores the potential of ML, combined with GPU optimization and model quantization, to accelerate conservative-to-primitive inversion in relativistic hydrodynamics simulations.
15 pages, 6 figures, 3 tables Manuscript content synced with publication
References in corpus (25)
- Color superconductivity in dense quark matter
- Equations of state for supernovae and compact stars
- Constraints on a phenomenologically parameterized neutron-star equation of state
- Three-dimensional GRMHD simulations of the remnant accretion disks from neutron star mergers: outflows and r-process nucleosynthesis
- Primitive Variable Solvers for Conservative General Relativistic Magnetohydrodynamics
- Prompt merger collapse and the maximum mass of neutron stars
- Binary Neutron Star Mergers
- Long-term GRMHD Simulations of Neutron Star Merger Accretion Disks: Implications for Electromagnetic Counterparts
- Constraining the neutron star equation of state with gravitational wave signals from coalescing binary neutron stars
- The Dynamics of Binary Neutron Star Mergers and of GW170817
- Low mass binary neutron star mergers : gravitational waves and neutrino emission
- Relativistic Magnetohydrodynamics In Dynamical Spacetimes: Numerical Methods And Tests
- General relativistic magnetohydrodynamic simulations of binary neutron star mergers forming a long-lived neutron star
- A New Open-Source Nuclear Equation of State Framework based on the Liquid-Drop Model with Skyrme Interaction
- Accretion-induced prompt black hole formation in asymmetric neutron star mergers, dynamical ejecta and kilonova signals
- Interpreting Binary Neutron Star Mergers: Describing the Binary Neutron Star Dynamics, Modelling Gravitational Waveforms, and Analyzing Detections
- Robust Recovery of Primitive Variables in Relativistic Ideal Magnetohydrodynamics
- Jet Launching from Binary Neutron Star Mergers: Incorporating Neutrino Transport and Magnetic Fields
- Numerical relativity simulations of the neutron star merger GW190425: microphysics and mass ratio effects
- Magnetohydrodynamic simulations of self-consistent rotating neutron stars with mixed poloidal and toroidal magnetic fields
- Machine Learning for Conservative-to-Primitive in Relativistic Hydrodynamics
- General Relativistic Hydrodynamics on a Moving-mesh I: Static Spacetimes
- Towards fidelity and scalability in non-vacuum mergers
- AsterX: a new open-source GPU-accelerated GRMHD code for dynamical spacetimes
- General relativistic magnetohydrodynamics simulations for binary neutron star mergers