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We study the evolution of planet-induced vortices in radially stratifieddisks, with initial conditions allowing for radial buoyancy. For this purposewe run global two dimensional hydrodynamical simulations, using the PLUTO code.Planet-induced vortices are a product of the Rossby wave instability (RWI)triggered in the edges of a planetary gap. In this work we assess the influenceof radial buoyancy for the development of the vortices. We found that radialbuoyancy leads to smoother planetary gaps, which generates weaker vortices.This effect is less pronounced for locally isothermal and quasi-isothermal(very small cooling rate) disks. We observed the formation of two generationsof vortices. The first generation of vortices is formed in the outer wall ofthe planetary gap. The merged primary vortex induces accretion, depleting themass on its orbit. This process creates a surface density enhancement beyondthe primary vortex position. The second generation of vortices arise in thissurface density enhancement, indicating that the bump in this region issufficient to trigger the RWI. The merged secondary vortex is a promisingexplanation for the location of the vortex in the Oph IRS48 system. Finally, weobserved a nonmonotonic behavior for the vortex lifetimes as a function of thethermal relaxation timescale, agreeing with previous studies. The birth timesof the secondary vortices also display a nonmonotonic behavior, which iscorrelated with the growth time of the primary vortex and its inducedaccretion.

Vortex Formation and Evolution in Planet Harboring Disks under Thermal Relaxation