A high-performance and portable asymptotic preserving radiation hydrodynamics code with the M₁ model

¹ Université Paris-Saclay, UVSQ, CNRS, CEA, Maison de la Simulation, 91191 Gif-sur-Yvette, France
e-mail: helene.bloch@cea.fr
² Université de Paris, AIM, 91191 Gif-sur-Yvette, France
³ AIM, CEA, CNRS, Université Paris-Saclay, 91191 Gif-sur-Yvette, France

Received: 4 June 2020
Accepted: 22 November 2020

Abstract

Aims. We present a new radiation hydrodynamics code called ARK-RT which uses a two-moment model with the M₁ closure relation for radiative transfer. This code was designed to be ready for high-performance computing on exascale architectures.

Methods. The two-moment model is solved using a finite-volume scheme. The scheme is designed to be asymptotic preserving in order to accurately capture both optically thick and thin regimes. We also propose a well-balanced discretization of the radiative flux source term which allows users to capture constant flux steady states with discontinuities in opacity. We use the library Trilinos for linear algebra and the package Kokkos allows us to reach high-performance computing and portability across different architectures, such as multi-core, many-core, and GP-GPU.

Results. ARK-RT is able to reproduce standard tests in both free-streaming and diffusive limits, including purely radiative tests and radiation hydrodynamics ones. Using a time-implicit solver is profitable as soon as the time-step given by the hydrodynamics is between 50 and 100 times larger than the explicit time-step for radiative transfer, depending on the preconditioner and the architecture. Nevertheless, more work is needed to ensure stability in all circumstances. Using ARK-RT, we study the propagation of an ionization front in convective dense cores. We show that the ionization front is strongly stable against perturbations even with destabilizing convective motions. As a result, the presence of instabilities should be interpreted with caution. Overall, ARK-RT is well-suited to studying many astrophysical problems involving convection and radiative transfer such as the dynamics of H II regions in massive pre-stellar dense cores and future applications could include planetary atmospheres.