<p>Protoplanetary disks, the sites of planet formation, are not necessarily symmetric. Observations in recent years even show that disks with non-axisymmetric features are common. Non-axisymmetric features could appear as bright arc-like structures or dark regions. Dark regions might be caused by a misaligned inner part of the disk casting a shadow onto the outer part. Such disks with a misaligned inner part are called <b>warped disks</b>. Possible reasons for a misalignment are a gravitational pull from an inclined planet, late infall of material onto the disk, or a change in direction of the angular momentum during the formation process.</p>
<p>To investigate the formation and evolution of warped disks, we developed the tool <i>dwarpy</i> for one-dimensional simulations. Such simulations are computationally less expensive than three-dimensional simulations and help provide valuable insight into how and when the observed shadows occur. To investigate the appearance of the shadows, we link dwarpy to RADMC-3D, a radiative transfer code, to create synthetic observations.</p>
<p>Additionally, we perform three-dimensional hydrodynamic simulations to test and compare to the one-dimensional description of the warped disk evolution. For this, we use FARGO3D, a grid-based hydrodynamic code. Testing the influence of the grid on the simulation outcome, we find that the grid effect can be restrained with a high enough resolution. We aim at simulating the effect of stellar fly-bys inclined with respect to the disk plane disks in 3D simulations.</p>