Speaker
Description
The formation of Warm Jupiters (with a period about 30 days and highly eccentric orbit (e > 0.3)) is still an open question. I investigated their possible early origins, ie. still embedded in the protoplanetary disk using numerical hydrodynamical simulations with the code GFARGO2. Assuming that planets are orbiting in the inner cavity of the disk, I found that planets can reach highly eccentric shrinking orbits. As a result, planets migrate under the Roche limit of the star and fall apart. This raises the question: is it possible for the planet to migrate into the cavity in the first place? Slight modification to the inner boundary condition of the hydrodynamic simulations allows the planet entering the inner cavity. However, in this case the eccentricity excitation stays moderate. My results indicate that further study requires the formation of Warm Jupiters.