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We perform a systematic study of the dynamics of dust particles inprotoplanetary disks with embedded planets using global 2-D and 3-D inviscidhydrodynamic simulations. Lagrangian particles have been implemented intomagnetohydrodynamic code Athena with cylindrical coordinates. We find twodistinct outcomes depending on the mass of the embedded planet. In the presenceof a low mass planet ($8 M_{\oplus}$), two narrow gaps start to open in the gason each side of the planet where the density waves shock. These shallow gapscan dramatically affect particle drift speed and cause significant, roughlyaxisymmetric dust depletion. On the other hand, a more massive planet ($>0.1M_{J}$) carves out a deeper gap with sharp edges, which are unstable to thevortex formation. Particles with a wide range of sizes ($0.02<\Omega t_{s}<20$)are trapped and settle to the midplane in the vortex, with the strongestconcentration for particles with $\Omega t_{s}\sim 1$. The dust concentrationis highly elongated in the $\phi$ direction, and can be as wide as 4 disk scaleheights in the radial direction. Dust surface density inside the vortex can beincreased by more than a factor of 10$^2$ in a very non-axisymmetric fashion.For very big particles ($\Omega t_{s}\gg 1$) we find strong eccentricityexcitation, in particular around the planet and in the vicinity of the meanmotion resonances, facilitating gap opening there. Our results imply that inweakly turbulent protoplanetary disk regions (e.g. the "dead zone") dustparticles with a very wide range of sizes can be trapped at gap edges andinside vortices induced by planets with $M_{p}<M_{J}$, potentially acceleratingplanetesimal and planet formation there, and giving rise to distinctivefeatures that can be probed by ALMA and EVLA.

Particle Concentration At Planet Induced Gap Edges and Vortices: I. Inviscid 3-D Hydro Disks