Here is a list of software projects that have been developed within the JHI.
Boris is a multi-physics software designed by JHI lecturer Dr Serban Lepadatu, to solve three-dimensional magnetisation dynamics problems, coupled with a self-consistent charge and spin transport solver, heat flow solver with temperature-dependent material parameters, and mechanical stress-strain solver in arbitrary multi-layered structures and shapes. The software is intended for research and design of spintronics devices, as well as analysis and modelling of experimental results.
Boris is now freely available for download, complete with a 170 pages manual and plenty of examples.
Summary of key features:
- CPU and GPU computations using CUDA
- Easy to use, as well as advanced control using Python scripting
- Thermoelectric and self-consistent spin transport solver integrated with magnetisation dynamics solver
- LLG and LLB simulations, including stochastic versions
- Multi-layered approach with independently discretized multiple computational meshes
- Temperature and spatially dependent material parameters allowing inclusion of defects, impurities, and physical roughness
- DMI, RKKY interaction, Oersted fields
- Domain wall and skyrmion tracking algorithms
- Spin transport solver allows computations with non-uniform charge and spin current densities, self-consistently including a number of effects: AMR, CPP-GMR, SHE, ISHE, spin pumping, bulk and interfacial spin torques.
An online application visualising the properties of a simulated galaxy.
Explore and visualise the effects of varying the wavelength and the inclination angle of a galaxy, and what can be observed at different wavelengths, and different angles. More information can be found here.
DART-Ray is a purely ray-tracing 3D dust radiative transfer code. It has been developed by Giovanni Natale while working in the research group of Cristina Popescu at the University of Central Lancashire between 2011 and 2017.
DART-Ray can be used to model the transport of stellar and dust emission within astrophysical objects taking into account the effect of interstellar dust including absorption, anysotropic scattering and re-emission. The dust emission can be calculated assuming dust at equilibrium with the radiation field or by performing a full calculation of the stochastically heated dust emission spectra. For any input arbitrary geometry of stellar and dust emission distributions, the code calculates the radiation field energy density distribution and the surface brightness maps as observed at arbitrary positions either far away or within the model. The code is written in Fortran 2003 and it is MPI+OpenMP parallelized. It allows to vary flexibly all the input physics (dust model, stellar emission SEDs) as well as the model geometry.