There is no author summary for this article yet. Authors can add summaries to their articles on ScienceOpen to make them more accessible to a non-specialist audience.
Abstract
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 with N-body simulations, including the type
I and II migration of planets, gas accretion of massive cores in a viscous disk. In
this paper, the standard formulations of type I and II migrations are adopted to investigate
the formation of planet systems around solar mass stars. Statistics on the final distributions
of planetary masses, semi-major axes and eccentricities are derived, which are comparable
to those of the observed systems. Our simulations predict some orbital signatures
of planet systems around solar mass stars: 36% of the survival planets are giant planets
(Mp>10Me). Most of the massive giant planets (Mp>30Me) locate at 1-10AU. Terrestrial
planets distribute more or less evenly at <1-2 AU. Planets in inner orbits (<1 AU)
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 MJ in highly eccentric orbits (e >
0.3 - 0.4). The average eccentricity (~ 0.15) of the giant planets (Mp>10Me) are bigger
than that (~ 0.05) of the terrestrial planets (Mp< 10Me). A planet system with more
planets tends to have smaller planet masses and orbital eccentricities on average.