A high-performance code for numerical simulations of astrophysical plasmas.
Documentation
GODUNOV and AMUN are numerical codes developed for high-resolution simulations of astrophysical flows within the fluid and magnetohydrodynamic (MHD) approximations. Both codes are designed to address a broad range of problems in computational astrophysics, including compressible hydrodynamics, magnetized plasmas, relativistic flows, and turbulence. They are based on modern finite-volume, Godunov-type numerical schemes, ensuring robust shock capturing and accurate treatment of discontinuities on structured meshes.
The GODUNOV code is a mature and well-tested framework for simulations on uniform grids, supporting hydrodynamic and magnetohydrodynamic equations in both classical and special relativistic regimes. It provides a flexible selection of numerical methods—such as different Riemann solvers, reconstruction schemes, and time integrators—while maintaining a relatively simple and transparent code structure. GODUNOV is written entirely in Fortran 2003 and supports MPI parallelization, making it suitable for efficient large-scale simulations on distributed-memory systems.
The AMUN code represents a more recent and actively developed framework, extending the capabilities of GODUNOV toward greater flexibility, higher-order accuracy, and modern high-performance computing environments. AMUN supports both uniform and adaptive meshes, advanced high-order reconstruction methods, embedded time integrators with error control, and hybrid MPI/OpenMP parallelism. Written in Fortran 2008, AMUN emphasizes modular design, scalability, and ease of extensibility, providing a powerful platform for current and future numerical studies in astrophysical fluid dynamics and plasma physics.
Documentation
GODUNOV and AMUN are numerical codes developed for high-resolution simulations of astrophysical flows within the fluid and magnetohydrodynamic (MHD) approximations. Both codes are designed to address a broad range of problems in computational astrophysics, including compressible hydrodynamics, magnetized plasmas, relativistic flows, and turbulence. They are based on modern finite-volume, Godunov-type numerical schemes, ensuring robust shock capturing and accurate treatment of discontinuities on structured meshes.
The GODUNOV code is a mature and well-tested framework for simulations on uniform grids, supporting hydrodynamic and magnetohydrodynamic equations in both classical and special relativistic regimes. It provides a flexible selection of numerical methods—such as different Riemann solvers, reconstruction schemes, and time integrators—while maintaining a relatively simple and transparent code structure. GODUNOV is written entirely in Fortran 2003 and supports MPI parallelization, making it suitable for efficient large-scale simulations on distributed-memory systems.
The AMUN code represents a more recent and actively developed framework, extending the capabilities of GODUNOV toward greater flexibility, higher-order accuracy, and modern high-performance computing environments. AMUN supports both uniform and adaptive meshes, advanced high-order reconstruction methods, embedded time integrators with error control, and hybrid MPI/OpenMP parallelism. Written in Fortran 2008, AMUN emphasizes modular design, scalability, and ease of extensibility, providing a powerful platform for current and future numerical studies in astrophysical fluid dynamics and plasma physics.