Formation of structures due to the presence of planets in the discs of young solar-like stars

Forming planets around young, fast-rotating, solar-like stars are exposed to strongly magnetized stellar winds, as a consequence of the enhanced magnetic activity of these stars. In addition to the action of these winds, transient energetic events such as coronal mass ejections (CMEs) are believed to be frequent in these environments, increasing the density, velocity, and magnetic field of the background stellar wind. The interaction between winds and CMEs, and the orbiting planets around active stars may lead to the formation of observable signatures due to the formation magnetic field and density disturbances in the vicinity these planets, such as comet-like tails or large bow shocks and may play a fundamental role in shaping the geometry of the possible present young planetary atmospheres. In this work, we study the interaction between the stellar winds of the very active, young star AB Doradus, a nearby young star, with a small rotation period (0.5 days) and a strong flaring activity, with unmagnetized planetary obstacles through numerical 2.5D simulations using the PLUTO MHD code.