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Abstract <p>Massive stars that form the Gould Belt OB associations are known to have higher multiplicity than solar-type stars. Due to their luminosity and close vicinity, they are optimal targets for speckle interferometry. Among the members of the Cas–Tau OB association, observed with the 6-m telescope of the Special Astrophysical Observatory of the Russian Academy of Sciences (BTA SAO RAS), a binary system, HI P10944 (B9VpSi, <InlineEquation ID="IEq1"> <EquationSource Format="TEX">\(G=5\overset{\textrm{m}}{.}53\)</EquationSource> <!--ASPBull2560066Butorina-m1--> </InlineEquation>), was discovered for the first time. We present the results of speckle interferometry monitoring of the star from 2007 to 2025, covering almost the entire orbital period (<InlineEquation ID="IEq2"> <EquationSource Format="TEX">\(P_{\textrm{orb}}=20.90\)</EquationSource> <!--ASPBull2560066Butorina-m2--> </InlineEquation> yrs). Based on the measured positional parameters, an orbit was constructed and the sum of the masses of the system’s components was determined (<InlineEquation ID="IEq3"> <EquationSource Format="TEX">\(M_{*}=4.26\pm 0.06M_{\odot}\)</EquationSource> <!--ASPBull2560066Butorina-m3--> </InlineEquation>).</p>

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Orbit of the Speckle Interferometric Binary System HIP 10944

  • 期刊论文

  • 发表日期：

    2025年12月1日

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  • M. D. Butorina,
  • V. V. Dyachenko,
  • A. S. Beskakotov,
  • A. A. Mitrofanova,
  • A. F. Maksimov,
  • Yu. Yu. Balega

摘要

Abstract

Massive stars that form the Gould Belt OB associations are known to have higher multiplicity than solar-type stars. Due to their luminosity and close vicinity, they are optimal targets for speckle interferometry. Among the members of the Cas–Tau OB association, observed with the 6-m telescope of the Special Astrophysical Observatory of the Russian Academy of Sciences (BTA SAO RAS), a binary system, HI P10944 (B9VpSi, \(G=5\overset{\textrm{m}}{.}53\) ), was discovered for the first time. We present the results of speckle interferometry monitoring of the star from 2007 to 2025, covering almost the entire orbital period ( \(P_{\textrm{orb}}=20.90\) yrs). Based on the measured positional parameters, an orbit was constructed and the sum of the masses of the system’s components was determined ( \(M_{*}=4.26\pm 0.06M_{\odot}\) ).