The Rossby wave instability and planet formation: 3D numerical simulations

Details The Rossby wave instability and planet formation: 3D numerical simulations The Rossby wave instability and planet formation: 3D numerical simulations

Nov 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008sf2a.conf..417m&link_type=abstract

"SF2A-2008: Proceedings of the Annual meeting of the French Society of Astronomy and Astrophysics Eds.: C. Charbonnel, F. Combes

Astronomy and Astrophysics

Astrophysics

Scientific paper

Models of planet formation do not explain yet the growth of planetesimals as in certain ranges of grain size collisions are too slow compared to estimated planet formation time. The Rossby wave instability (RWI) may solve this problem by the formation of Rossby vortices in the accretion disc, speeding up the accumulation of grains in their centre ( te{Peggy} ). Up to now, only two dimensions numerical studies of the RWI have been done. In this proceeding we present the results of three dimensions numerical simulations of the non-linear evolution of the RWI in a non magnetized disc and its vertical structure.

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