Post-Oligarchic Evolution of Protoplanetary Embryos and the Stability of Planetary Systems

Details Post-Oligarchic Evolution of Protoplanetary Embryos and the Stability of Planetary Systems Post-Oligarchic Evolution of Protoplanetary Embryos and the Stability of Planetary Systems

2007-05-15

arxiv.org/abs/0705.2164v1

Astrophys.J.666:423-435,2007

Astronomy and Astrophysics

Astrophysics

15 pages, 13 figures (2 color ones), accepted for publication in ApJ

Scientific paper

10.1086/519918

We investigate the orbit-crossing time (T_c) of protoplanet systems both with and without a gas-disk background. The protoplanets are initially with equal masses and separation (EMS systems) scaled by their mutual Hill's radii. In a gas-free environment, we find log (T_c/yr) = A+B \log (k_0/2.3). Through a simple analytical approach, we demonstrate that the evolution of the velocity dispersion in an EMS system follows a random walk. The stochastic nature of random-walk diffusion leads to (i) an increasing average eccentricity ~ t^1/2, where t is the time; (ii) Rayleigh-distributed eccentricities (P(e,t)=e/\sigma^2 \exp(-e^2/(2\sigma^2)) of the protoplanets; (iii) a power-law dependence of T_c on planetary separation. As evidence for the chaotic diffusion, the observed eccentricities of known extra solar planets can be approximated by a Rayleigh distribution. We evaluate the isolation masses of the embryos, which determine the probability of gas giant formation, as a function of the dust and gas surface densities.

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