20 Orbits of binaries based on soar speckle observations

被引：4

作者：

Gomez, Jorge ^{[1
,2
,3
]}

Docobo, Jose A. ^{[1
,2
,3
,4
]}

Campo, Pedro P. ^{[1
,2
,3
]}

Andrade, Manuel ^{[1
,2
,3
,5
]}

Mendez, Rene A. ^{[6
]}

Costa, Edgardo ^{[6
]}

机构：

[1] Univ Santiago de Compostela USC, Observ Astron Ramon Maria Aller, Ave Ciencias S-N,Campus Vida, E-15782 Santiago De Compostela, Galiza, Spain

[2] USC, Inst Matemat, Fac Matemat, Rua Lope Gomez de Marzoa S-N,Campus Vida, E-15782 Santiago De Compostela, Galiza, Spain

[3] USC, Dept Matemat Aplicada, Fac Matemat, Rua Lope Gomez de Marzoa S-N,Campus Vida, E-15782 Santiago De Compostela, Galiza, Spain

[4] Fac Ciencias, Real Acad Ciencias Zaragoza, C Pedro Cerbuna 12, E-50009 Zaragoza, Spain

[5] USC, Escola Politecn Super Enxenaria, Benigno Ledo S-N,Campus Terra, E-27002 Lugo, Galiza, Spain

[6] Univ Chile, Casilla 36-D, Santiago, Chile

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2022年 / 509卷 / 03期

关键词：

techniques: high angular resolution; astrometry; binaries: visual; stars: fundamental parameters; STAR CD-ROM; VISUAL BINARIES; SPECTRAL TYPES; CATALOG; MASSES; INTERFEROMETRY; CLASSIFICATION; LUMINOSITIES;

D O I：

10.1093/mnras/stab2633

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

New observational data obtained during the 2018, 2019, and 2020 speckle runs with the 4.1-m Southern Astrophysical Research (SOAR) telescope located at Cerro Pachon (Chile) allowed us to recalculate the orbits of the visual binaries: WDS 00277-1625 (YR 1 Aa,Ab), WDS 00462-2214 (RST4155), WDS 03124-4425 (JC 8), WDS 07427-3510 (HDS 1091), WDS 10093+2020 (A2145), WDS 10116+1321 (HU 874 AB), WDS 10217-0946 (BU 25), WDS 11585-2350 (RST 3767 AB), WDS 13117-2633 (FIN 305), WDS 13305+0729 (A 1789), and WDS 16458-0046 (A1141). In addition, we present the first orbits calculated for the following binaries: WDS 07303-5657 (FIN 105), WDS 09110-1929 (I 824), WDS 12111-5302 (HU 1604), WDS 14592-4206 (HDS 2116 Aa,Ab), WDS 15157-2736 (BU 350), WDS 15493+0503 (A 1126), WDS 16402-2800 (VOU 44 AB), and WDS 18126+1224 (HDS 2570). All of them are placed below Dec. + 21 degrees and the majority are main-sequence stars. Except in cases with giant components or close triple systems, the ANAPAR method was used in order to obtain precise dynamical parallaxes and individual masses. These parallaxes were compared with those obtained by Gaia and/or Hipparcos satellites. In the case of FIN 305, we present two different orbital solutions. Also, using the dynamical parallaxes given by these orbits, we have been able to calculate the luminosity of these systems. Said luminosities allow us to indicate an approximate age for the components of these systems, situating them within the Hertzsprung-Russell (HR) diagram. In addition, a commentary for each binary about the physical and dynamical properties of the studied binaries has been included.

引用

页码：4229 / 4245

页数：17

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