Orbits and masses in two triple systems

被引:0
作者
Nazor, Dinko [1 ]
Tokovinin, Andrei [2 ]
机构
[1] Pixel Ribs Doo, Vlaska 79, Zagreb 10000, Croatia
[2] Cerro Tololo Interamer Observ NSFs NOIRlab, Casilla 603, La Serena, Chile
基金
美国国家航空航天局;
关键词
binaries: spectroscopic; binaries: visual; stars: individual: HIP 86286; stars: individual: HIP 117258; SPECKLE INTERFEROMETRY; STARS; CATALOG; MODELS; TESS; SOAR;
D O I
10.1093/mnras/stae2400
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
In an effort to determine accurate orbital and physical properties of a large number of bright stars, a method was developed to fit simultaneously stellar parameters (masses, luminosities, effective temperatures), distance, and orbits to the available data on multiple systems, namely the combined and differential photometry, positional measurements, radial velocities (RVs), accelerations, etc. The method is applied to a peculiar resolved triple system HIP 86286. The masses of its components estimated using observations and standard relations are 1.3, 0.9, and 0.9 M-circle dot; the main star is a G8IV subgiant, while its two companions are main-sequence dwarfs. The inner and outer orbital periods are 35 and 287 yr, respectively, and the orbits are nearly coplanar. The second system, HIP 117258, is an accelerating star with a resolved companion; its 35.7-yr orbit based on relative astrometry and precise RVs yields the secondary mass of 0.95 M-circle dot, much larger than inferred from the photometry. The apparent paradox is explained by assuming that the secondary is a close pair of M-type dwarfs with yet unknown period.
引用
收藏
页码:976 / 981
页数:6
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