Structure of the Stellar Neighborhood of CQ Tau in the Presence of a Companion in an Elongated Orbit

Abstract

There are indirect signs of the presence of a companion near the star CQ\,Tau. A period of 10\;years was found in the brightness changes. The image of the disk shows an extensive cavity with a size of about 25~AU, surrounded by a dust ring with a distribution maximum near 53~AU. A simulation of the interaction of dust and gas in the vicinity of the star with the CQ\,Tau parameters was carried out, assuming the existence of a companion in an orbit with a period of 10\;years. It was shown that an M-class star in a highly elongated orbit is capable of forming a region of reduced density around the center of mass of the system, with a size close to the observed one. However, the dust ring-like structure in this case is located noticeably closer to the star than observed. Evidence has been obtained that a massive planet in an outer, relatively binary orbit, could form a ring-shaped dust structure at a distance similar to that observed.