The Rossby wave instability in 2D viscous protoplanetary discs

Details The Rossby wave instability in 2D viscous protoplanetary discs The Rossby wave instability in 2D viscous protoplanetary discs

Dec 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011sf2a.conf..469c&link_type=abstract

SF2A-2011: Proceedings of the Annual meeting of the French Society of Astronomy and Astrophysics Eds.: G. Alecian, K. Belkacem,

Astronomy and Astrophysics

Astrophysics

1

Scientific paper

To form meter-sized pre-planetesimals in protoplanetary discs, dust aggregates have to collide at velocities lower than a threshold so that they are not destroyed during the collision. Dust grains are affected by the gas through aerodynamic drag, therefore its study is relevant in determining the grain growth evolution. The Rossby Wave Instability tep[RWI, non-axisymetric instability,][]{LC99, LH78}, may solve this problem by the formation of vortices where dust particles can accumulate, collide at low velocity and stick together tep{BS95}. We study the development of the RWI in a 2D viscous disc using the Smoothed Particle Hydrodynamics (SPH) method. We show that Rossby Vortices can form and survive in the disc for a few thousand years. The instability is triggered by a ``jump'' in the radial surface density profile caused by the presence of a dead zone in the protoplanetary disc.

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