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.

arXiv comment14 pages, 9 figures, 1 table

References in corpus (23)

• The cosmological simulation code GADGET-2
• Disk Frequencies and Lifetimes in Young Clusters
• GADGET: A code for collisionless and gasdynamical cosmological simulations
• Protoplanetary Disks and Their Evolution
• Smoothed Particle Hydrodynamics and Magnetohydrodynamics
• Coagulation, fragmentation and radial motion of solid particles in protoplanetary disks
• Dust coagulation in protoplanetary disks: a rapid depletion of small grains
• Dust Migration and Morphology in Optically Thin Circumstellar Gas Disks
• A Millimeter Continuum Size-Luminosity Relationship for Protoplanetary Disks
• Dust retention in protoplanetary disks
• How not to build Tatooine: the difficulty of in situ formation of circumbinary planets Kepler 16b, Kepler 34b and Kepler 35b
• Circumbinary Planet Formation in the Kepler-16 system. I. N-body Simulations
• Planetary chaotic zone clearing: destinations and timescales
• A dust and gas cavity in the disc around CQ Tau revealed by ALMA
• Kepler-16b: safe in a resonance cell
• A highly non-Keplerian protoplanetary disc: Spiral structure in the gas disc of CQ Tau
• Three-lane and multi-lane signatures of planets in planetesimal disks
• External or internal companion exciting the spiral arms in CQ Tau?
• Photometric activity of CQ Tau on the time interval of 125 years
• Long-Term Dynamics of Planetesimals in Planetary Chaotic Zones
• Simulations of the dynamics of the debris disks in the systems Kepler-16, Kepler-34, and Kepler-35
• "Horseshoe" Structures in the Debris Disks of Planet-Hosting Binary Stars
• SPH simulations of structures in protoplanetary disks