Solar System Dynamics at the Last Stage of Planetary Formation (by invitation)

PARISI, M. G.; BRUNINI, A.

San Pablo, Brasil

Conferencia; X Coloquio Brasilero de Dinamica Orbital (CBDO2000); 2000

UNESP

On one hand, the upper limit of the mass distribution of planetesimals at the end of the formation of the planets is obtained. The determination of the masses of the largest bodies which are out of the distribution due to runaway accretion is included. On the other hand, we set dynamical constraints to the Uranian system, assuming that the large spin axis inclination of Uranus (98 degrees) is due to the great Collision hypothesis. The impulse imparted by this collision had strongly to affect the dynamical characteristics of preexisting outer satellites. The discovery of the five outer Uranian moons (Gladman et al 1998, 2000) sets important constraints in this scenario.