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Abstract <p>The list of brown dwarfs (BD) for which spatial coordinate and velocity components were found (<i>n</i>&#xa0;= 13) was compiled using the catalog (Reylé et al. 2021, <i>r</i> &lt; 10 pc from the Sun). Numerical calculations of the orbits of the BD in our list were performed using the classical galaxy model. The distribution of the majority of BD in our list in terms of orbital eccentricity (<i>e</i>) were in the narrow range <i>e</i> = 0.04–0.16, which indicates a relatively uniform age of most objects and their belonging to the same kinematic subsystem. An exception is the object Gaia EDR3 ID 1589250088362827776, the kinematics of which (<i>e</i> = 0.41) indicates that it possibly belongs to a halo. The <i>Z</i><sub>max</sub> distribution showed that the overwhelming majority of BD in our list are part of the “thin” disk population with <i>Z</i><sub>max</sub> &lt; 600 pc. The study is partially based on a talk presented at the Modern Stellar Astronomy 2025 conference.</p>

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Kinematics of Brown Dwarfs in the Solar Vicinity

  • 期刊论文

  • 发表日期：

    2025年12月1日

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  • E. S. Postnikova,
  • M. D. Sizova,
  • T. Bugra Keskin,
  • N. V. Chupina,
  • S. V. Vereshchagin

摘要

Abstract

The list of brown dwarfs (BD) for which spatial coordinate and velocity components were found (n = 13) was compiled using the catalog (Reylé et al. 2021, r < 10 pc from the Sun). Numerical calculations of the orbits of the BD in our list were performed using the classical galaxy model. The distribution of the majority of BD in our list in terms of orbital eccentricity (e) were in the narrow range e = 0.04–0.16, which indicates a relatively uniform age of most objects and their belonging to the same kinematic subsystem. An exception is the object Gaia EDR3 ID 1589250088362827776, the kinematics of which (e = 0.41) indicates that it possibly belongs to a halo. The Zmax distribution showed that the overwhelming majority of BD in our list are part of the “thin” disk population with Zmax < 600 pc. The study is partially based on a talk presented at the Modern Stellar Astronomy 2025 conference.