Theoretical models of planetary system formation: mass vs. semi-major axis

摘要: Context. Planet formation models have been developed during the past years to try reproduce what has observed of both solar system and extrasolar planets. Some these partially succeeded, but they focus on massive planets and, for sake simplicity, exclude belonging planetary systems. However, more are now found in This tendency, which is a result radial velocity, transit, direct imaging surveys, seems be even pronounced low-mass These new observations require improving planet models, including physics, considering systems. Aims: In recent series papers, we presented some improvements physics our focussing particular internal structure forming planets, computation excitation state planetesimals their resulting accretion rate. this paper, concurrent effect than one same protoplanetary disc show effect, terms architecture composition multiplicity. Methods: We used an N-body calculation collision detection compute orbital evolution system. Moreover, describe competition gas solids, as well gravitational interactions between planets. Results: that masses semi-major axes modified by interactions. also present assumed number (a free parameter model), inclination eccentricity damping. find fraction ejected increases from nearly 0 8% change embryos seed with 2 20 embryos. calculations that, when ~5 M⊕, simulations 10 or statistically give results mass function period distribution.