Protoplanetary disks are commonly found in the initial stages of star evolution. Young low mass stars, such as T Tauri, are exhaustively studied to constrain the different processes within protoplanetary disks. In this context, planet-disk interactions processes are crucial for understanding the role of planets in the evolution of the disk. Dust trapping, shoulder, spiral arms or gaps are structures and features of protoplanetary disks that can be explained by planets. Just as planets produce effects on the gas and dust, the latter also influence the planets, such as in the case of planet accretion, resonances, effects in the semimajor axis and eccentricity.

In particular the well-studied PDS 70 system, with its two directly imaged protoplanets, illustrates how planets can induce significant changes in the disk, such as a large gap of 60 AU and notable dust segregation. Nevertheless, the less massive and more common brown dwarfs (BD) present new challenges and opportunities. Since their formation mechanism is similar to that of the stars, BDs have protoplanetary disks at the beginning of their evolution. Their low mass disks, typically in a range of 0.5 to 3 Earth masses, makes it difficult to form massive planets and, in consequence, substructures from planet-disk interactions. However, young brown dwarfs and proto-BD are expected to form massive planets. Proto-BD observations suggest an initial disk mass of around 20-30 Mj, allowing the formation of Saturn-mass planets in early stages of the disk. This type of planets trigger planet-disk interaction processes as gaps or dust trapping.

In this test using 2D simulations with FARGO3D, we compare planet-disk interaction processes in T Tauri stars and BDs, analyzing the structures formed by planet-disk interaction, such as millimeter dust trapping and gap formation, looking for analogous mechanisms in these similar regimes. We explore whether a planet with the mass of Mercury can accrete enough gas to grow into a Saturn-mass planet and consequently carve a gap in a BD disk, inspecting the gas accretion rate and dust distribution during the evolution from proto-BD to 0.1 Myr BD disk.