目视双星ADS 8119 AB（α = 11 h 18 m 10 s.9，δ=+31 o31 '44”.9）的轨道

视双星轨道和质量确定的计算算法

Computational Algorithm for Orbit and Mass Determination of Visual Binaries

本文介绍了一种确定视双星轨道根数和质量的算法。该算法使用一个最佳点，它最小化一个特定的函数描述的最小二乘解和精确解之间的平均长度。要最小化的目标函数是精确的，没有任何近似。该算法适用于Kowalsky的方法的轨道参数计算，和里德的方法确定的动力学视差和个人的群众。该程序适用于A 1145和ADS 15182。

The First Dynamical Mass Determination of a Nitrogen-rich Wolf-Rayet Star using a Combined Visual and Spectroscopic Orbit

We present the first visual orbit for the nitrogen-rich Wolf-Rayet binary, WR 133 (WN5o + O9I) based on observations made with the CHARA Array and the MIRC-X combiner. This orbit represents the first visual orbit for a WN star and only the third Wolf-Rayet star with a visual orbit. The orbit has a period of 112.8 d, a moderate eccentricity of 0.36, and a separation of $a$= 0.79 mas on the sky. We combine the visual orbit with an SB2 orbit and Gaia parallax to find that the derived masses of the component stars are $M_{\rm WR}$ = $9.3\pm1.6 M_\odot$ and $M_{\rm O}$ = $22.6\pm 3.2 M_\odot$, with…

Visual Orbits of Spectroscopic Binaries with the CHARA Array. II. The eclipsing binary HD 185912

We present the visual orbit of the double-lined eclipsing binary, HD 185912, from long baseline interferometry with the CHARA Array. We also obtain echelle spectra from the Apache Point observatory to update the spectroscopic orbital solution and analyze new photometry from Burggraaff et al. to model the eclipses. By combining the spectroscopic and visual orbital solutions, we find component masses of M1 = 1.361 +/- 0.004 Msun and M2 = 1.331 +/- 0.004 Msun, and a distance of d = 40.75 +/- 0.30 pc from orbital parallax. From the light curve solution, we find component radii of R1 = 1.348 +/- 0.…

“快”视双星的散斑干涉测量和轨道

Speckle interferometry and orbits of "fast" visual binaries

报告了2012年4.1米SOAR望远镜的散斑观测结果（121个系统的158个测量值，27个非分辨率）。目的是跟踪最近发现或被忽视的近距离双星和子系统的快速轨道运动。在这里，8个以前已知的轨道被更好地定义，两个完全修订，并首次计算了五个轨道。利用依巴谷天体或散斑天体的差分测光以及质量和绝对星等之间的标准关系，对所有15个具有新轨道或更新轨道的系统，估算了其组成部分的质量和动力学弛豫。首次分辨出HIP 54214和HIP 56245两颗天体测量双星，并测量了另外8颗。我们强调几个未解决的对，实际上可能是单一的，尽管有多个历史措施，如104头和f小狗AB。需要继续监测，以了解这些神秘的案件。

Estimation of the masses of selected stars of Pulkovo program by means of astrometry methods

Stars of Pulkovo observatory program are observed on 65-cm refractor during many years for study their positions and movement. We represent example of two visual binary stars, for which orbits and masses of components were determined, and two astrometric stars, for which masses of their unseen companions have been estimated. The first stars are: ADS 14636 (61 Cygni) and ADS 7251 and others are: Gliese 623 and ADS 8035 (Alpha UMa). The direct astrometric methods were used for estimation of mass-ratio and masses.

The orbits of visual binary and multiple stars obtained by the Apparent Motion Parameters method during the last 40 years

Summed many years of work at Pulkovo, the orbits of 67 wide pairs of visual double and multiple stars (included in 64 systems) which were obtained by the Apparent Motion Parameters (AMP) method are presented. This short arc determination orbit method is based on the most reliable astrometric and astrophysical data corresponding to one instant of time. The rest of the observations accumulated in the world serve to control the quality of the orbit and refine some parameters. All early determined AMP-orbits were compared with new observations, some of them were recalculated, new ones were added. …

Visual Orbits of Spectroscopic Binaries with the CHARA Array. I. HD 224355

We present the visual orbit of the double-lined spectroscopic binary HD 224355 from interferometric observations with the CHARA Array, as well as an updated spectroscopic analysis using echelle spectra from the Apache Point Observatory 3.5m telescope. By combining the visual and spectroscopic orbital solutions, we find the binary components to have masses of M1 = 1.626 +/- 0.005 Msun and M2 = 1.608 +/- 0.005 Msun, and a distance of d = 63.98 +/- 0.26 pc. Using the distance and the component angular diameters found by fitting spectrophotometry from the literature to spectral energy distribution…

目视双星WDS 17190-3459的轨道和物理参数（α 2000 = 17 h 18 m 56 s，δ 2000 = -34 o 59' 22”）

Orbital and Physical Parameters of Visual Binary: WDS 17190-3459 (α 2000 = 17h 18m 56s and δ 2000 = - 34o 59' 22")

自1923年Bosscha天文台建立以来，对可见双星的研究在印度尼西亚的天文学研究中发挥了重要作用。我们的天文台和其他天文台广泛地观测到了这对目视双星：WDS 17190-3459 = MLO 4AB = HD 156384 = HIP 84709。该系统自1876年底观测以来，已经三次通过近星点。观测数据足以构建一个轨道。用Thiele-Innes方法计算了其轨道，用质光关系确定了其物理参数。结果见下表。轨道参数：e = 0.578，P = 42.3年，T = 1974.9，i = 132 o.7，ω = 247 o.5，Ω = 318 o.1，a = 1”.713，mu = 8 o.51/年物理参数：p = 0”.134，Mbol 1 = 6.7，Mbol 2 = 7.4，M1 = 0.6 Mo，M2 = 0.5 Mo，q = 0.863。目前有几种新的方法来确定轨道;例如Söderhjelm（1999）的高斯方法，用于计算同一颗恒星的轨道WDS 17190-3459。我们的结果相对相同。

行星宿主双星系统的视觉轨道与对齐

Visual Orbits & Alignments of Planet Hosting Binary Systems

本研究通过高分辨率成像测量13个行星宿主双星系统的视觉轨道，发现双星轨道与凌星行星轨道高度对齐，补充了盖亚对宽距双星的研究。

The spin-orbit alignment of visual binaries

The angle between the stellar spin-axis and the orbital plane of a stellar or planetary companion has important implications for the formation and evolution of such systems. A study by Hale (1994) found that binaries with separations $a < 30$ au are preferentially aligned while binaries on wider orbits are frequently misaligned. We aim to test the robustness of the Hale (1994) results by reanalysing the sample of visual binaries with measured rotation periods using independently derived stellar parameters and a Bayesian formalism. Our analysis is based on a combination of data from Hale (1994)…