Magnetohydrodynamics (MHD)

Magnetohydrodynamics (MHD) is the study of magnetic fluids and gives a good description of the dynamics of the Sun's atmosphere. MHD wave theory is a rich and fascinating area of study because, by the nature of the supporting plasma, it is based on the interplay of three different modes, namely Alfvén, fast and slow magnetoacoustic waves.

Our research primarily focuses on the mathematical modelling of solar and astrophysical processes. Current research focuses on: (i) understanding the physics of the solar chromosphere using advanced computational models, large-scale simulations and solar observations; (ii) particle acceleration, including the use of particle-in-cell (PIC) numerical techniques; and (iii) MHD wave propagation in inhomogeneous media, including detecting and tracking solar MHD waves, where high-resolution observations reveal dynamic behaviour and magnetic waves throughout all layers of the Sun's atmosphere.

We answer fundamental questions using advanced mathematical techniques and cutting-edge computer simulations, including the use of high-performance computing. We also exploit the latest high-resolution data taken with international ground-based and spaced-based instruments to study the dynamical events occurring in the solar atmosphere (members of the group have co-investigator status on a number of international missions/instruments).

Case Study: Northumbria University researcher inspires physics students