Self-sustaining vortices in protoplanetary discs: Setting the stage for planetary system formation

The core accretion scenario of planet formation assumes that planetesimals and planetary embryos are formed during the primordial, gaseous phases protoplanetary disk. However, how dust particles overcome traditional growth barriers is not well understood. recently proposed viscous ring-instability may explain concentric rings observed in disks by assuming grains can reduce gas conductivity, which weaken magneto-rotational instability. We present an analysis this model with help GPU-based numerical hydrodynamic simulations coupled thin-disk limit. During evolution disk dusty become Rossby unstable break up into a cascade small-scale vortices. vortices form secularly stable structures, could be sites planetesimal streaming instability as direct gravitational collapse. phenomenon self-sustaining consistent observational constraints exoplanets sets favorable environment for system formation.