Abstract
We review vortex formation through instabilities associated with structural features in protoplanetary disks. We then describe the form of the generic parametric or elliptical instability associated with and, localized on, non circular streamlines. The effect of this type of instability on the potential accumulation of solid particles in the centre of such vortices has yet to be determined.
Highlights
Planets are believed to form in circumstellar disks of gas and dust circulating around around young stars
Large-scale, long-lived vortices may play an important role in this process, since gas drag can result in them collecting solid particles in their centres (Barge & Sommeria 1995) potentially speeding up the accumulation process (Lyra et al 2009)
The generation of vortices through instabilities at gap edges induced by orbiting planets, or at an interface between a live and dead zone, or through amplification through the subcritical baroclinic instability has been shown to be robust. The centres of such vortices have been proposed be the sites of concentration of solid particles that migrate there through the action of gas drag
Summary
Planets are believed to form in circumstellar disks of gas and dust circulating around around young stars. Large-scale, long-lived vortices may play an important role in this process, since gas drag can result in them collecting solid particles in their centres (Barge & Sommeria 1995) potentially speeding up the accumulation process (Lyra et al 2009). Such vortices require a driving process to maintain them against known potential instabilities and viscous decay. Possible processes involve instabilities associated with features in the protoplanetary disk such as rings and gaps and baroclinic effects. We discuss these here as well as the ideas behind possible parametric or elliptical instabilities associated with non circular streamlines
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