Radial Distribution of Planets. Predictions based on the Core Accretion Gas Capture Planet formation Model

摘要

We have investigated the problem of the distribution of both masses andorbital radii of planets resulting from the gas-accretion, gas-capture model.First we followed the evolution of gas and solids from the moment where allsolids are in the form of small grains to the stage when most of them are inthe form of planetesimals for a set of different initial masses and sizes ofprotoplanetary disks. Based on that we performed Monte Carlo calculationsdescribing the formation of giant places at different locations. We includedthe effects of type II migration and growth of the mass of the planet after thegap opened. We discuss how these effects influence the final distribution ofgiant planets. We show that when the giant planets are not able to migrate orgrow in mass after the gap opens, their distribution is mainly determined bythe properties of the gaseous disk. However, with those two effects included,reproducing the parameters of the gaseous disks from the distribution ofplanets becomes difficult. We also checked the roles of both the material ofwhich the solids consist and the mass of the central star. The main result isthat, in disks around less massive stars, giant planets at the given locationtend to be less massive. At the same time, the giant planets with the givenmass tend to form closer to the less massive stars.