During the late stage of planet formation when Mars-sized cores appear , interactions among planetary cores can excite their orbital eccentricities , accelerate their mergings and thus sculpture their final orbital architecture .
This study contributes to the final assembling of planetary systems with N-body simulations , including the type I or II migrations of planets , gas accretion of massive cores in a viscous disk .
Statistics on the final distributions of planetary masses , semimajor axes and eccentricities are derived , which are comparable to those of the observed systems .
Our simulations predict some new orbital signatures of planetary systems around solar mass stars : 36 \% of the survival planets are giant planets ( > 10 M _ { \oplus } ) .
Most of the massive giant planets ( > 30 M _ { \oplus } ) locate at 1-10AU .
Terrestrial planets distribute more or less evenly at < 1 - 2 AU .
Planets in inner orbits may accumulate at the inner edges of either the protostellar disk ( 3-5 days ) or its MRI dead zone ( 30-50 days ) .
There is a planet desert in the mass-eccecntricity diagram , i.e. , lack of planets with masses 0.005 - 0.08 M _ { J } in highly eccentric orbits ( e > 0.3 - 0.4 ) .
The average eccentricity ( \sim 0.15 ) of the giant planets ( > 10 M _ { \oplus } ) is bigger than that ( \sim 0.05 ) of the terrestrial planets ( < 10 M _ { \oplus } ) .
A planetary system with more planets tends to have smaller planet masses and orbital eccentricities on average .