This is a project which is currently making use of HPC facilities at Newcastle University. It is active.
For further information about this project, please contact:
This project involves simulations of magnetohydrodynamical phenomena in the solar interior, focusing particularly upon the dynamics of the solar tachocline and the lower convection zone, and the possible role that the tachocline might be playing in the generation of the large-scale solar magnetic field.
This project uses our compressible magnetohydrodynamics code (P3D), which is written in Fortran and parallelised using MPI. This code utilises a mixed pseudo-spectral/finite-difference scheme for the spatial derivatives, with FFTW being used to calculate the required discrete Fourier transforms. Data snapshots are producing using the NetCDF self-describing data format.