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We use a multi-dimensional hydrodynamics code to study the gravitationalinteraction between an embedded planet and a protoplanetary disk with emphasison the generation of vortensity (potential vorticity) through a BaroclinicInstability and subsequent development of Rossby-Wave-Instability (RWI). It isfound that the generation of potential vorticity is very common and effectivein non-barotropic disks through the Baroclinic Instability, especially withinthe coorbital region. Our results also complement previous studies by\citet{KLL03} that non-axisymmetric RWIs are likely to develop at local minimaof potential vorticity distribution that are generated by the interactionbetween a planet and a inviscid barotropic disk. This second instabilityappears to be very common and robust, regardless of the equation of state,initial density distribution, and rotational law of the disk. The developmentof RWIs results in non-axisymmetric density blobs, which exert stronger torquesonto the planet when they travel in the vicinity of the planet. As a result ofthat, large amplitude oscillations are introduced to the time behavior of thetotal torque acted on the planet by the disk. In our current simulations, RWIsdo not change the overall picture of inward orbital migration but bring in anon-monotonic behavior to the migration speed. As a side effect, RWIs alsointroduce interesting structures into the disk. These structures may help theformation of Earth-like planets in the Habitable Zone or Hot Earths interior toa close-in giant planet.

Disk-Planet Interaction Simulations: (I) Baroclinic Generation of Vortensity and Non-Axisymmetric Rossby-Wave-Instability