The solar atmosphere hosts rotating magnetised plasma flow structures that channel energy and waves from the solar surface into the corona. Understanding how these swirling structures reorganise magnetic fields and drive energy upward is key to solving one of solar physics’ greatest puzzles: why the corona is millions of degrees hotter than the surface?

This PhD project will investigate how swirling plasma motions interact with magnetic fields to regulate energy transport across solar atmospheric layers. You will analyse cutting-edge solar observations, combined with state-of-the-art high-performance computing magnetohydrodynamic (MHD) simulations. Using advanced automated detection techniques, you will identify and study coherent magnetic and flow structures that dominate energy transfer and quantify the associated Poynting flux.

Based within the Plasma Dynamics Group (PDG, https://pdg.sites.sheffield.ac.uk/home) at the University of Sheffield, you will gain expertise in solar observations, numerical modelling, and plasma physics while contributing to breakthrough research on solar atmospheric coherent structures, coronal heating, and solar wind acceleration.

The PhD studentship, funded by the STFC, is intended for home students graduating in a relevant subject (Mathematics, Physics, Astronomy/Astrophysics, etc.). It includes full UK tuition fees, a living allowance (stipend), and additional funding to cover research costs, collaborative visits, and national and international travel to conferences and workshops.

Application Deadline: March 13th, 2026 (please note the very tight deadline)
Expected Start Date: October 2026

For further information, details on the project and application procedure, please contact Prof. Viktor Fedun (v.fedun@sheffield.ac.uk).