Formation of TRAPPIST-1

TRAPPIST-1 is a nearby 0.08 solar mass M-star, which was recently found to harbor a planetary system of at least seven ~Earth-mass planets, all residing within 0.1 au. The configuration is not easily explained by either the in situ or migration model for planet formation. I will present an alternative scenario for the formation and orbital architecture of the TRAPPIST-1 system. In this model, planets form at the H2O iceline (~0.1 au for the Trappist-1 disk) and is fueled by the migration of pebble-size particles from the outer disk. I will argue that this pebble accretion is particularly efficient for low stellar masses as Trappist-1. With some adjustment, the model can also be applied to compact systems of more massive stars, i.e., that many close-in super-Earth systems can be regarded as a scaled-up version of TRAPPIST-1.

Chris Ormel — API, UvA
Thursday 15 June 2017, 12:00
Location: C4.174