Dynamical Evolution of Planetesimals in the Solar Nebula

Details Dynamical Evolution of Planetesimals in the Solar Nebula Dynamical Evolution of Planetesimals in the Solar Nebula

Sep 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996dps....28.1115k&link_type=abstract

American Astronomical Society, DPS meeting #28, #11.15; Bulletin of the American Astronomical Society, Vol. 28, p.1109

Astronomy and Astrophysics

Astronomy

1

Scientific paper

We investigate the dynamical evolution of planetesimals in the solar nebula using 3-D N-body calculation. The gas drag due to the solar nebula is taken into account. We assume that the gas velocity is about 0.2% slower than the circular velocity. In the solar nebula, the velocity dispersion (eccentricity and inclination) of planetesimals are raised by gravitational scattering among planetesimals and are damped by the gas drag due to the solar nebula. The magnitude of the velocity dispersion and its distribution governs the mode and the time scale of planetary accretion. The equilibrium values of the RMS eccentricity and the RMS inclination are investigated. We find that the equilibrium values well agree with the values obtained from the analytical arguments. The distribution functions of the eccentricity and the inclination is also investigated. We find that the eccentricity and the inclination are not co-related. Adopting the Kolmogonov-Smirnov test, we show that the distribution functions of the eccentricity and the inclination of planetesimals are well agree with Gaussian distribution. We present the result of the distribution of planetesimals around a protoplanet. The accretion of planetesimals in the solar nebula is also investigated. We discuss the effect of gas drag on planetary accretion.

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