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Gas rich dusty circumstellar discs observed around young stellar objects arebelieved to be the birthplace of planets and planetary systems. Recentobservations revealed that large-scale horseshoe-like brightness asymmetriesare present in dozens of transitional protoplanetary discs. Theoretical studiessuggest that these brightness asymmetries bf could be caused by large-scaleanticyclonic vortices triggered by the Rossby Wave Instability (RWI), which canbe excited at the edges of the accretionally inactive region, the dead zoneedge. Since vortices may play a key role in planet formation, investigating theconditions of the onset of RWI and the long-term evolution of vortices isinevitable. The aim of our work was to explore the effect of disc geometry (thevertical thickness of the disc), viscosity, the width of the transition regionat the dead zone edge, and the disc mass on the onset, lifetime, strength andevolution of vortices formed in the disc. We performed a parametric studyassuming different properties for the disc and the viscosity transition byrunning 1980 2D hydrodynamic simulations in the locally isothermal assumptionwith disc self-gravity included. Our results revealed that long-lived,large-scale vortex formation favours a shallow surface density slope and low-or moderate disc masses with Toomre $Q \lesssim 1/h$, where $h$ is thegeometric aspect ratio of the disc. In general, in low viscosity models,stronger vortices form. However, rapid vortex decay and re-formation is morewidespread in these discs.

On the evolution of vortex in locally isothermal self-gravitating discs: a parameter study