Abstract
Numerical simulations of merging compact objects and their remnants form the theoretical foundation for gravitational wave and multimessenger astronomy. While Cartesian-coordinate-based adaptive mesh refinement is commonly used for simulations, spherical-like coordinates are more suitable for nearly spherical remnants and azimuthal flows due to lower numerical dissipation in the evolution of fluid angular momentum, as well as requiring fewer numbers of computational cells. However, the use of spherical coordinates to numerically solve hyperbolic partial differential equations can result in severe Courant-Friedrichs-Lewy (CFL) stability condition time step limitations, which can make simulations prohibitively expensive. This paper addresses this issue for the numerical solution of coupled spacetime and general relativistic magnetohydrodynamics evolutions by introducing a double fast Fourier transform (FFT) filter and implementing it within the fully message passing interface (mpi)-parallelized sphericalnr framework in the einstein toolkit. We demonstrate the effectiveness and robustness of the filtering algorithm by applying it to a number of challenging code tests, and show that it passes these tests effectively, demonstrating convergence while also increasing the time step significantly compared to unfiltered simulations.
| Original language | English |
|---|---|
| Article number | 104005 |
| Journal | Physical Review D |
| Volume | 108 |
| Issue number | 10 |
| DOIs | |
| State | Published - Nov 15 2023 |
Funding
The authors would like to thank Thomas W. Baumgarte, Pablo Cerdá-Durán, Luciano Combi, Eirik Endeve, Roland Haas, J. Austin Harris, W. Raphael Hix, Jay V. Kalinani, Eric Lentz, Carlos O. Lousto, Jens F. Mahlmann, O. E. Bronson Messer, Scott C. Noble, Martin Obergaulinger, David Radice, and Erik Schnetter for useful discussions. We gratefully acknowledge the National Science Foundation (NSF) for financial support from Grants No. PHY-2110338, No. OAC-2004044/1550436, No. AST-2009330, No. OAC-1811228, and No. PHY-1912632 to RIT; as well as Grants No. PHY-1806596, PHY-2110352, and OAC-2004311 to U. of Idaho. We gratefully acknowledge NASA for financial support from Grants No. NASA NNH17ZDA001N-TCAN-17-TCAN17-0018 80NSSC18K1488 to RIT, and No. ISFM-80NSSC18K0538 to U. of Idaho. V. M. is supported by the Exascale Computing Project (17-SC-20-SC), a collaborative effort of the U.S. Department of Energy (DOE) Office of Science and the National Nuclear Security Administration. Work at Oak Ridge National Laboratory is supported under Contract No. DE-AC05-00OR22725 with the U.S. Department of Energy. Computational resources were provided by TACC’s Frontera supercomputer allocations (Grants No. PHY-20010 and No. AST-20021). Additional resources were provided by RIT’s BlueSky and Green Pairie and Lagoon Clusters acquired with NSF Grants No. PHY-2018420, No. PHY-0722703, No. PHY-1229173, and No. PHY-1726215. Funding for computer equipment to support the development of senr/nrpy+ was provided in part by NSF EPSCoR Grant No. OIA-1458952 to West Virginia University. All plots in this paper were created using m atplotlib for which we have used the pyc actus to import carpet data.
| Funders | Funder number |
|---|---|
| National Science Foundation | PHY-2110338, OAC-1811228, PHY-1806596, OAC-2004311, AST-2009330, OAC-2004044/1550436, PHY-2110352, PHY-1912632 |
| U.S. Department of Energy | |
| National Aeronautics and Space Administration | 17-SC-20-SC, NNH17ZDA001N-TCAN-17-TCAN17-0018 80NSSC18K1488, ISFM-80NSSC18K0538 |
| Office of Experimental Program to Stimulate Competitive Research | OIA-1458952 |
| Office of Science | |
| National Nuclear Security Administration | DE-AC05-00OR22725, PHY-1726215, PHY-20010, PHY-1229173, AST-20021, PHY-0722703, PHY-2018420 |