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Abstract <p>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 variations. 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 a star with 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-type 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 one observed. 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 elongated orbit, could form a ring-shaped dust structure at a distance similar to that observed.</p>

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

  • 期刊论文

  • 发表日期：

    2025年3月1日

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  • T. V. Demidova

摘要

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 variations. 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 a star with 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-type 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 one observed. 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 elongated orbit, could form a ring-shaped dust structure at a distance similar to that observed.