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Abstract <p>Based on the catalog ([<CitationRef CitationID="CR5">5</CitationRef>], <InlineEquation ID="IEq1"> <EquationSource Format="TEX">\(r&lt;10\)</EquationSource> <!--BPhysMGU2570122Postnikova-m1--> </InlineEquation> pc from the Sun), a list of brown dwarfs (BDs) was compiled for which it was possible to find components of spatial coordinates and velocity (<InlineEquation ID="IEq2"> <EquationSource Format="TEX">\(n=13\)</EquationSource> <!--BPhysMGU2570122Postnikova-m2--> </InlineEquation>). Within the framework of the classical model of the Galaxy, numerical calculations of the orbits of BDs from our list were carried out. The distribution by orbital eccentricity (e) turned out to be on a narrow interval, which indicates a small spread in the ages of BDs. An exception is Gaia EDR3 ID 1589250088362827776, the kinematics of which (<InlineEquation ID="IEq3"> <EquationSource Format="TEX">\(e=4.1\)</EquationSource> <!--BPhysMGU2570122Postnikova-m3--> </InlineEquation>) indicates that it may belong to the halo. The distribution by <InlineEquation ID="IEq4"> <EquationSource Format="TEX">\(Z_{\textrm{max}}\)</EquationSource> <!--BPhysMGU2570122Postnikova-m4--> </InlineEquation> showed that the BDs from our list are part of the population of the ‘‘thin’’ disk with <InlineEquation ID="IEq5"> <EquationSource Format="TEX">\(Z_{\textrm{max}}&lt;600\)</EquationSource> <!--BPhysMGU2570122Postnikova-m5--> </InlineEquation> pc.</p>

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Characteristics of the Brown Dwarf Population in the Vicinity of the Sun

  • 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

Based on the catalog ([5], \(r<10\) pc from the Sun), a list of brown dwarfs (BDs) was compiled for which it was possible to find components of spatial coordinates and velocity ( \(n=13\) ). Within the framework of the classical model of the Galaxy, numerical calculations of the orbits of BDs from our list were carried out. The distribution by orbital eccentricity (e) turned out to be on a narrow interval, which indicates a small spread in the ages of BDs. An exception is Gaia EDR3 ID 1589250088362827776, the kinematics of which ( \(e=4.1\) ) indicates that it may belong to the halo. The distribution by \(Z_{\textrm{max}}\) showed that the BDs from our list are part of the population of the ‘‘thin’’ disk with \(Z_{\textrm{max}}<600\) pc.