  High resolution ALMA observations revealed a variety of rich substructures in
numerous protoplanetary disks. These structures consist of rings, gaps and
asymmetric features. It is debated whether planets can be accounted for these
substructures in the dust continuum. Characterizing the origin of asymmetries
as seen in HD 163296 might lead to a better understanding of planet formation
and the underlying physical parameters of the system. We test the possibility
of the formation of the crescent-shaped asymmetry in the HD 163296 disk through
planet-disk interaction. The goal is to obtain constraints on planet masses and
eccentricities and disk viscosities. Two dimensional, multi-fluid,
hydrodynamical simulations are performed with the FARGO3D code including three
embedded planets. Dust is described with the pressureless fluid approach and is
distributed over eight size bins. Resulting grids are post-processed with the
radiative transfer code RADMC-3D and the CASA software to model synthetic
observations. We find that the crescent-shaped asymmetry can be qualitatively
modeled with a Jupiter mass planet at a radial distance of 48 au. Dust is
trapped preferably in the trailing Lagrange point L5 with a mass of 10 to 15
earth masses. Increased values of eccentricity of the innermost Jupiter mass
planet damages the stability of the crescent-shaped feature and does not
reproduce the observed radial proximity to the first prominent ring in the
system. Generally, a low level of viscosity ($\alpha \leq 2\cdot10^{-3}$) is
necessary to allow the existence of such a feature. Including dust feedback the
leading point L4 can dominantly capture dust for dust grains with an initial
Stokes number $\leq 3.6\cdot 10^{-2}$. The observational results suggest a
negligible effect of dust feedback since only one such feature has been
detected so far.
