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During the late stage of planet formation when Mars-size cores appear,interactions among planetary cores can excite their orbital eccentricities,speed their merges and thus sculpture the final architecture of planet systems.This series of work contributes to the final assembling of planet systems withN-body simulations, including the type I and II migration of planets, gasaccretion of massive cores in a viscous disk. In this paper, the standardformulations of type I and II migrations are adopted to investigate theformation of planet systems around solar mass stars. Statistics on the finaldistributions of planetary masses, semi-major axes and eccentricities arederived, which are comparable to those of the observed systems. Our simulationspredict some orbital signatures of planet systems around solar mass stars: 36%of the survival planets are giant planets (Mp>10Me). Most of the massive giantplanets (Mp>30Me) locate at 1-10AU. Terrestrial planets distribute more or lessevenly at <1-2 AU. Planets in inner orbits (<1 AU) may accumulate at the inneredges of either the protostellar disk (3-5 days) or its MRI dead zone (30-50days). There is a planet desert in the mass-eccecntricity diagram, i.e., lackof planets with masses 0.005 - 0.08 MJ in highly eccentric orbits (e > 0.3 -0.4). The average eccentricity (~ 0.15) of the giant planets (Mp>10Me) arebigger than that (~ 0.05) of the terrestrial planets (Mp< 10Me). A planetsystem with more planets tends to have smaller planet masses and orbitaleccentricities on average.

Modeling Planetary System Formation with N-Body Simulations: Role of Gas Disk and Statistics Comparing to Observations