Séminaire : Relating protoplanetary disks to exoplanets: from models to space observations.

Planetary embryos are formed in protoplanetary disks that have not reached their steady state yet. Therefore, modeling the disk and its viscous evolution is crucial for understanding where and when exoplanets will form. I developed a new hydrodynamical code to model consistently the disk dynamics, thermodynamics, geometry and composition all together. This code was tested against previous semi-analytical disk models and retrieved the observed characteristics of protoplanetary disks. In addition, this model takes into account the disk self-shadowing.

In this talk, I will describe how viscously evolved disk profiles present temperature plateaus located at the sublimation lines of the various dust elements. In particular, I will detail how planets migrate in such disks and in which case they may be trapped and saved at a specific location varying with the disk profile and with the planet mass. I will also explicit which traps are transient, which ones are sustainable and which ones may lead to gap opening.

I will present possible applications of this work regarding CAIs formation and future space missions. On a short term basis, generating simulated observations of protoplanetary disks from numerical models will help analyze the future JWST-MIRI observations and reconstruct the observed disks. On a longer term, as planet traps are the preferred locations for exoplanets to grow, it is essential to determine the genetic relationship between protoplanetary disks and their exoplanets. In the scope of the PLATO mission, detecting exoplanets and potentially exomoons will greatly benefit from protoplanetary disks models. Finally, modeling the icy satellite formation in circumplanetary disks will provide models for the galilean satellites interior that the JUICE mission will be able to constrain.