Planet formation models: the interplay with the planetesimal disc

摘要: Context. According to the sequential accretion model (or core-nucleated model), giant planet formation is based first on of a solid core which, when massive enough, can gravitationally bind gas from nebula form envelope. The most critical part time core: trigger gas, has grow up several Earth masses before component protoplanetary disc dissipates. Aims: We calculate planetary models including detailed description dynamics planetesimal disc, taking into account both drag and excitation forming planets. Methods: computed planets, considering oligarchic regime for growth core. Embryos growing in stir their neighbour planetesimals, exciting relative velocities, which makes more difficult. Here we introduce realistic treatment evolution planetesimals' directly impact timescale. For this, state as result stirring by gas-solid interactions. Results: find that planets favoured small random velocities are easily damped nebula. Moreover, capture radius protoplanet with (tiny) envelope also larger planetesimals. However, migrate disc-planet angular momentum exchange, important consequences survival: due slow regime, rapid inward type I migration implications intermediate-mass have not yet started runaway phase gas. Most these lost central star. Surviving either below 10 M⊕ or above Jupiter masses. Conclusions: To dissipation planetesimals (~0.1 km) be major contributors process. combination fast leads absence planets. Other processes must therefore at work explain population extrasolar presently known.