Planets are believed to form in an environment called a protoplanetary disk (PPD), a structure of gas and dust rotating around protostars. In this early epoch, not only does this vicinity influence the planets’ composition and accretion processes, a planet or planetary core itself has a potential impact on changing and shaping the surrounding material. Even though the gas considerably dominates the total mass of the disk, the comparably small amount of dust can play a crucial role. First, most planetforming processes depend on the dynamics of the dust. On top of this, when investigating PPDs, the information we can infer is strongly biased towards the dust content. Like this, the best-resolved observations are obtained from the dust continuum emission and also the study of meteorites only directly exposes the solid content of the early Solar System. This thesis investigates the impact of planets onto the surrounding dust structure and how these modifications of the PPD can lead to observable or measurable signatures. It employs an interdisciplinary approach, combining theory, cosmochemistry and telescope observations, in order to validate and falsify specific scenarios. The dynamics of dust is strongly influenced by the collisional friction with the local gaseous material. In an unperturbed disk model, in which temperature and gas density are monotonously increasing towards the star, dust experiences a drift that is directed radially inwards. The first project discusses how a giant planet impacts the radial transport of solids in a PPD. For this, we perform a set of numerical simulations including gas and multiple dust species and investigate, how, and how much, dust is transported from an initially outer reservoir to parts of the disk that are closer to the star than the planet’s orbit. We find, that while small particles are allowed to enter this inner zone, solids that are larger than a critical size are filtered out by the perturbations that the planet introduces in the gas structure – they accumulate at the outer edge of a gap that the planet creates in the disk. Subsequently, we test how this critical grain size changes for important model parameters. Our own Solar System contains two giant planets, Jupiter and Saturn, that must have formed early after the Sun’s formation, more than four and a half billion years ago. Therefore, the filtration found from our numerical results should have occurred around the Sun when the PPD there was still present. This filtration had significant effects on the composition of bodies that formed in environments inside and outside of Jupiter’s (and Saturn’s) orbit. We inspect such a body by scanning the inner Solar System chondrite NWA 5697 – a meteorite that contains pristine material that formed within the circumsolar disk, and thus partly conserves the conditions present there. It has been assumed from previous studies that chondrites linked to the inner Solar System do not contain certain components found in the outer Solar System, such as calcium-aluminium-rich inclusions (CAIs). This was often imputed to the impact of Jupiter on dust transport to the inner system. Yet, motivated by the results from numerical simulations, we found small CAIs in this inner Solar System chondrite, which were previously not resolved. Indeed, this detection supports the idea of Jupiter being responsible for the meteoritic dichotomy in the Solar System. Additionally, it allows us to investigate some crucial parameters of the early circumsolar disk. We infer essential disk quantities, such as viscosity and gas abundance, and inspect different constellations between Jupiter and Saturn. In a second part, we investigate the signature that an intermediate-mass planet imposes onto the dust structure of the disk, in case that the body is continuously changing its semi-major axis. This behaviour is known as planet migration and is predicted from numerous theoretical investigations. We model the reaction of the PPD to several different migration scenarios in a disk of a low level of viscosity. Again, we employ hydrodynamical simulations of the gas and five different dust species. In most cases, the planet creates multiple circular, concentric dust enhancements in- and around its orbit. This dust structure is prone to be affected by the planet’s migration rate. By performing radiative transfer simulations and subsequent image synthesis, we show that this effect is observable with the Atacama Large Millimeter/submillimeter Array (ALMA). Thus, this may link highly resolved future observations to the planetary migration state, and therefore to an important open question of planet formation. With these projects, this thesis tries to answer some fundamental questions about the history of our Solar System and planetary behaviour in faraway PPDs. It outlines, how the link of different disciplines, such as theory, observations and cosmochemistry, can lead to a better constraint of prevailing conditions present at the times and places of planet formation. This knowledge is substantialfor a thorough understanding of planet formation itself.