Relativistic Dirac R-matrix photoionisation calculations through to their implementation with stellar opacity
codes

To understand stellar opacities and hence stellar environments, a robust understanding of the atomic/molecular processes and constituents present is required. My work involves utilising parallel FORTRAN-based supercomputing to model atomic data required for radiative processes in stars – processes often fundamental to how these objects exist and evolve. Dependant on atomic number, this relies on either semi-relativistic Breit-Pauli or fully relativistic Dirac models – starting from first principles and collaborating with experimental projects to produce high quality atomic data for astrophysically relevant conditions and elements. Atomic data produced can then be integrated with radiative transport codes, often in stellar or high-energy contexts such as SNe Ia, to better interpret astronomical observations and advance theoretical understanding.

Biography

Originally from Buckinghamshire, I began my PhD in September 2020 following graduation from QUB with a MSci in Physics. My Master’s Project focused on Python and C-based radiative transport codes to evaluate the potential impact of the Local Thermodynamic Equilibrium approximation in the context of SNe Ia. I also focused in carbon in these SNe as a trace for explosion models. My undergraduate experiences revealed an interest in computationally intensive work and theoretical modelling. As such, I have had ample opportunities to access leading computational facilities in the UK and Germany, and further study radiation-driven environments at a fundamental level. Recreationally, I enjoy reading, coding, and various sports such as volleyball or archery.

Research interests

• Radiative Transfer
• Astronomical Spectroscopy
• Computational Astrophysics
• R-Matrix Theory
• High Performance Computing