Journal
ASTRONOMY & ASTROPHYSICS
Volume 659, Issue -, Pages -Publisher
EDP SCIENCES S A
DOI: 10.1051/0004-6361/202142557
Keywords
hydrodynamics; convection; turbulence; stars; interiors; methods; numerical
Categories
Funding
- US Department of Energy through the Los Alamos National Laboratory (LANL)
- National Nuclear Security Administration of the US Department of Energy [89233218CNA000001]
- Klaus Tschira Foundation
- German Research Foundation (DFG) [RO 3676/3-1]
- Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) [EXC 2181/1 -390900948]
- Gauss Centre for Supercomputing e.V.
- NSERC Discovery Grant
- JINA Center for the Evolution of the Elements (NSF) [PHY-1430152]
- NSF [PHY-1430152, 1814181, 2032010]
- ERC [787361-COBOM]
- consolidated STFC grant [ST/R000395/1]
- BEIS capital funding via STFC capital grants [ST/K000373/1, ST/R002363/1, ST/P002293/1, ST/R002371/1]
- STFC DiRAC Operations grant [ST/R001014/1, ST/K003267/1]
- World Premier International Research Centre Initiative (WPI Initiative), MEXT, Japan
- IReNA AccelNet Network of Networks - National Science Foundation [OISE-1927130]
- COST (European Cooperation in Science and Technology) [CA16117]
- European Union [101008324]
- Durham University
- STFC [ST/R000832/1]
- BIS National E Infrastructure capital grant [ST/K00042X/1]
- STFC capital grants [ST/H008519/1, ST/K00087X/1]
- Australian Research Council [FT160100046, DP190102431]
- Australian Government
- Government of Western Australia
- Australian Research Council [FT160100046] Funding Source: Australian Research Council
- Direct For Mathematical & Physical Scien
- Division Of Astronomical Sciences [1814181] Funding Source: National Science Foundation
- Office of Advanced Cyberinfrastructure (OAC)
- Direct For Computer & Info Scie & Enginr [2032010] Funding Source: National Science Foundation
Ask authors/readers for more resources
Our ability to predict the structure and evolution of stars is limited by complex hydrodynamic processes. However, our simulations show that hydrodynamic simulations of flows in stellar interiors are reliable.
Our ability to predict the structure and evolution of stars is in part limited by complex, 3D hydrodynamic processes such as convective boundary mixing. Hydrodynamic simulations help us understand the dynamics of stellar convection and convective boundaries. However, the codes used to compute such simulations are usually tested on extremely simple problems and the reliability and reproducibility of their predictions for turbulent flows is unclear. We define a test problem involving turbulent convection in a plane-parallel box, which leads to mass entrainment from, and internal-wave generation in, a stably stratified layer. We compare the outputs from the codes FLASH, MUSIC, PPMSTAR, PROMPI, and SLH, which have been widely employed to study hydrodynamic problems in stellar interiors. The convection is dominated by the largest scales that fit into the simulation box. All time-averaged profiles of velocity components, fluctuation amplitudes, and fluxes of enthalpy and kinetic energy are within less than or similar to 3 sigma of the mean of all simulations on a given grid (128(3) and 256(3) grid cells), where sigma describes the statistical variation due to the flow's time dependence. They also agree well with a 512(3) reference run. The 128(3) and 256(3) simulations agree within 9% and 4%, respectively, on the total mass entrained into the convective layer. The entrainment rate appears to be set by the amount of energy that can be converted to work in our setup and details of the small-scale flows in the boundary layer seem to be largely irrelevant. Our results lend credence to hydrodynamic simulations of flows in stellar interiors. We provide in electronic form all outputs of our simulations as well as all information needed to reproduce or extend our study.
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