TAPIR Seminar

Our own Solar System contains planets on relatively circular orbits, but this assertion is far from being true for the majority of exoplanetary systems. However, one thing extrasolar systems have in common with the Solar System (and are expected to) is the prominence of mean-motion resonances. But what happens when mean-motion resonances involve eccentric planets? 
In this seminar, I will present two of my recent work on these aspects and show how analytical arguments, and in particular phase-space diagrams, can guide and complement numerical simulations to unravel mechanisms which can explain for instance the extremely eccentric orbit of Fomalhaut b, or the presence of exozodiacal clouds in mature systems.