Connecting planetary properties with formation in evolving protoplanetary disks
With the discovery of thousands of exoplanets that comprise several distinct planetary populations, we have learned a great deal about planetary masses and their orbital radii (the M-a diagram), as well as some idea of their composition, structure and planetary atmospheres (the M-R diagram). ALMA observations, meanwhile, are starting to uncover the physical properties of disks, rings, and gaps that allow us to probe how planets are formed. All of this provides important constraints on how planetary properties arise from their formation. In this talk, I address the current observations and ideas of planet formation, migration, and composition. I will show that radial drift of dust in disks as well as disk sizes strongly impact how and where planets form. By comparing comprehensive planetary population synthesis and disk astrochemistry calculations with observed M-a and M-R diagrams, we can begin to predict planetary structural and atmospheric properties. Among our major results is a surprising link between the size and nature of SuperEarth and warm Jovian planet populations.
|Date: ||Jeudi, le 3 octobre 2019|
|Lieu: ||Université de Montréal|
| ||Roger-Gaudry, D-460|
|Contact: ||RenÃ© Doyon|