In recent years ALMA imaging of protoplanetary discs has revealed a broad and beautiful range of structures and morphologies alerting us to the underlying mechanisms of planet formation. Despite this variety, we can identify some trends that begin to reveal to us the nature of planet formation, one such trend is with the mass of the stellar host. In this seminar I will present results from my work that uses the structure, evolution and mass of protoplanetary discs to study how the mechanisms of planet formation differ depending on the stellar host.
Mass of the central object is linked to the mass of the planet-building material, the size of the disc, and observational results suggest a link to disk lifetime as well. Furthermore, the evolution of stellar luminosity during the disc-hosting phase alters disc mid-plane temperature suggesting temporal variations of disc composition for any given orbital radius in the disc. I will present modelling of protoplanetary discs using self-consistent calculations of mid-plane temperature that suggest a dichotomy in the temperature, and subsequently the composition, of disc mid-planes around low and intermediate mass stars. Applying this modelling to the HR8799 planetary system, we can explore what constraints can be placed on both where and when giant planets in the system may have formed.