3:45 PM - 4:00 PM
[PCG19-18] Orbital Distribution of Gas Giants from Dust-to-Planet Simulations.
Keywords:planet formation, gas giant planet, planetary accretion
Gas-giant planets, such as Jupiter, Saturn and massive exoplanets, were formed via the gas accretion onto the solid cores each with a mass roughly ten times that of Earth. However, rapid radial migration due to tidal disk interaction occurs prior the formation of such massive cores via the accretion of planetesimals. In spite of all our efforts, planetesimal formation, planetary migration, and gas-giant core formation have been major challenges for planet formation models. We recently developed the new simulation method to treat full
collisional evolution from dust to planets in a whole disk, called dust-to-planet simulation (DTPS). As a result of DTPSs, cores are formed inside 10 au in several 10^5 years, because pebbles grow into planetesimals via collisions prior to drift in 10 au. The rapid core formation occurs independent of porosity of pebbles, unless disk temperatures are extremely high. Core formation occurs in 1–10 au according to the masses and temperatures of disks. Gas giants comparable to or smaller than Jupiter are expected to migrate insignificantly. Such gas giants have orbits similar to the birth orbits of cores.
collisional evolution from dust to planets in a whole disk, called dust-to-planet simulation (DTPS). As a result of DTPSs, cores are formed inside 10 au in several 10^5 years, because pebbles grow into planetesimals via collisions prior to drift in 10 au. The rapid core formation occurs independent of porosity of pebbles, unless disk temperatures are extremely high. Core formation occurs in 1–10 au according to the masses and temperatures of disks. Gas giants comparable to or smaller than Jupiter are expected to migrate insignificantly. Such gas giants have orbits similar to the birth orbits of cores.