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Abstract <p>The paper presents orbits of 69 wide pairs of visual binary and multiple stars (belonging to 65 systems) obtained by the Apparent Motion Parameters (AMP) method. The possibility of determining the AMP orbits of these pairs using Gaia DR3 data at the time point 2016.0 is considered. (1) Orbits according to Gaia DR3 were obtained for 45 pairs. (2) For another 20 pairs, the quasi-instantaneous motion according to Gaia data contradicts the mean motion from all available observations. A possible reason is the presence of inner subsystems. (3) AMP orbits were also determined for 3 bright stars (ADS 2080, ADS 7724, and ADS 9173) and 3 close pairs (angular separation less than <InlineEquation ID="IEq1"> <InlineMediaObject> <ImageObject Color="BlackWhite" FileRef="11444_2025_1684_Article_IEq1.gif" Format="GIF" Height="15" Rendition="HTML" Resolution="72" Type="Linedraw" Width="18" /> </InlineMediaObject> <EquationSource Format="TEX">\(2'' \)</EquationSource> <!--AstEng2570180Romanenko-m1--> </InlineEquation>: ADS 2416, ADS 5570, and T Tau NS) that do not have the Gaia DR3 positional observations. The basis for the study in cases 2 and 3 is the Pulkovo series of observations on the 26-inch refractor and/or data from the literature. Of the 69 pairs of stars studied, 59 have semi-major axes of the orbit greater than 100 AU. Among them, families of orbits with minimum periods from 5000 to 730 000 years and minimum semi-major axes of more than 400 AU were obtained for 17 pairs. Unique solutions were obtained for the orbits of 28 pairs. Of these, 20 pairs have a semi-major axis of the orbit greater than 100 AU and periods from 600 to 6000 years. Relative errors in determining the elements are generally about 15–20%. The orientation of the resulting orbits in the Galactic coordinate system is also determined.</p>

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The Pulkovo Catalog of the Orbits Obtained for Visual Binary and Multiple Stars by the Apparent Motion Parameters Method

  • 期刊论文

  • 发表日期：

    2025年5月1日

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  • L. G. Romanenko,
  • O. V. Kiyaeva,
  • I. S. Izmailov,
  • N. A. Shakht,
  • D. L. Gorshanov

摘要

Abstract

The paper presents orbits of 69 wide pairs of visual binary and multiple stars (belonging to 65 systems) obtained by the Apparent Motion Parameters (AMP) method. The possibility of determining the AMP orbits of these pairs using Gaia DR3 data at the time point 2016.0 is considered. (1) Orbits according to Gaia DR3 were obtained for 45 pairs. (2) For another 20 pairs, the quasi-instantaneous motion according to Gaia data contradicts the mean motion from all available observations. A possible reason is the presence of inner subsystems. (3) AMP orbits were also determined for 3 bright stars (ADS 2080, ADS 7724, and ADS 9173) and 3 close pairs (angular separation less than \(2'' \) : ADS 2416, ADS 5570, and T Tau NS) that do not have the Gaia DR3 positional observations. The basis for the study in cases 2 and 3 is the Pulkovo series of observations on the 26-inch refractor and/or data from the literature. Of the 69 pairs of stars studied, 59 have semi-major axes of the orbit greater than 100 AU. Among them, families of orbits with minimum periods from 5000 to 730 000 years and minimum semi-major axes of more than 400 AU were obtained for 17 pairs. Unique solutions were obtained for the orbits of 28 pairs. Of these, 20 pairs have a semi-major axis of the orbit greater than 100 AU and periods from 600 to 6000 years. Relative errors in determining the elements are generally about 15–20%. The orientation of the resulting orbits in the Galactic coordinate system is also determined.