The effect of photoevaporation on the evolution of migrating giant planets

In the last few decades our understanding of young planet formation and evolution has been greatly improved by many observations of planets with Kepler and TESS and discs with ALMA. This is being complemented by intense research into planet-disc interactions, specifically through the increasing use of hydrodynamical simulations. This research aims to characterise the behaviour of multi-planet systems of giant planets in protoplanetary discs. This is relevant as most systems harbour multiple planets and with the release of astrometry data by Gaia in the next few years we expect to discover a few thousand of such giant planet systems. It is then extremely important to understand the orbital evolution theory of these systems. This work uses the Fargo3d hydrodynamical simulation code to investigate the effect of photoevaporation from the central star on disc resonances, specifically on how it affects the evolution of planetary eccentricities once they are trapped in a resonance. This research also characterises how photoevaporation changes migration rates and resonance trapping timescales, by affecting the disc mass loss rate within the disc gaps.