Modelling Protoplanetary Discs Using 3D Radiative Transfer

Planets form in protoplanetary discs, large discs of gas and dust surrounding young stars. In this thesis, I developed and applied radiative transfer models to simulate molecular line emission from such discs, and compare these simulations directly with radio observations from the Atacama Large Millimeter/submillimeter Array (ALMA). By fitting models to the data, I explored the physical and chemical structure of discs, including temperature, turbulence, and the distribution of different molecules. This work helps us understand the environments in which planets form and how young planets may influence their birthplaces.