Gravitational Instability and Clustering in a Disk of Planetesimals

Details Gravitational Instability and Clustering in a Disk of Planetesimals Gravitational Instability and Clustering in a Disk of Planetesimals

May 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004dda....35.0205t&link_type=abstract

American Astronomical Society, DDA meeting #35, #02.05; Bulletin of the American Astronomical Society, Vol. 36, p.851

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The real importance of the gravitational instability in the dust disk of the early Solar System is still debated. Several mechanisms could yield a strongly inhomogeneus distribution of solids: radial drift, trapping in vortices, perturbations by massive bodies, etc. Some of them could be relevant in the formation of planets around the Sun or other stars. Here we present a numerical study of a gravitationally unstable layer. Numerical limitations impose the use of large bodies, resulting in a strong gravitational stirring. However, a simple method allows us to control the growth of velocity dispersions and to explore the highly non-linear evolution of the instably layer. A hierarchical growth of structures in presence of gas drag can yield large clusters of planetesimals, inside which particle growth take place.

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