The PDG group carries out fundamental research in the stability, dynamics, structure, and evolution of astrophysical fluids
(heliospheric and stellar interiors and atmospheres, together with their environments) and laboratory plasmas (magnetically confined fusion).
Our research relies heavily on analytical methods, state-of-the-art numerical modelling (HPC and GPU computing), as well as
observations and laboratory experiments with the aim to give answers to crucial questions such as:
- how is the plasma in solar and stellar atmospheres heated to million degrees (by linear and nonlinear waves, magnetic reconnection/diffusion, turbulences);
- how the various regions in these atmosphere are coupled;
- how instabilities affect the evolution of energy and the flux of plasmas;
- how small scale processes (such as turbulences and waves) affect the dynamical and thermal state of the plasma and structure;
- how magnetic fields are generated through dynamo processes, and what is their evolution in different astrophysical objects;
- how to improve the confinement of plasmas in laboratory devices;
- how ionospheric perturbations can help us to predict natural hazards: application to climate prediction and natural hazard risk assessment.