Dynamical study of the wide visual binary ADS 12815 (16 Cyg)

Kiselev, A. A.; Romanenko, L. G.

doi:10.1134/s1063772911060059

Cited by 198 publications

(9 citation statements)

References 2 publications

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“…In some cases, an excess of mass was detected. In this way, the presence of a third companion was confirmed for some stars, such as, for example, ADS 497 and ADS 11061, see Kiselev & Romanenko (1996); Kisselev & Kiyaeva (2004) and Tokovinin & Smekhov (2002).…”

Section: Data Processingmentioning

confidence: 86%

“…To determine the orbits of binary stars, we apply the apparent motion parameters (AMP) method developed in Pulkovo, which was repeatedly used to determine the orbits of satellites and asteroids from observations on a relatively short arc tracing the orbit, see Kiselev & Romanenko (1996). We also applied this method to estimating the black hole mass at the center of our Galaxy in the system consisting of the black hole and star S01 revolving around the dynamic center, see Kisselev et al (2007).…”

Section: History and Observationsmentioning

confidence: 99%

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Estimating masses of selected stars in the Pulkovo program by means of astrometry methods

Shakht

Gorshanov

Vasilkova

2018

Res. Astron. Astrophys.

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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. ADS 7251 INTRODUCTIONThe mass of the star is one of its most important characteristics. Amount of matter in a star determines its temperature and pressure in the center, and also determines other characteristics of the star and then its evolutionary path. Direct estimates of the mass of the star are made on the basis of the law of universal gravitation.The study of binary stars has allowed to establish the unity of Newton's laws in the Universe and to obtain the fundamental knowledge about the masses of stars on the basis of observations. The determination of the masses of the stars by classic way is done by means of positional astrometric observations of double stars with the high-precision instruments for a long time. Observations should cover a long time interval, or the period of revolution of a double star must be sufficiently short compared to the total observation period. We also need the exact value of the distances for stars and that means -the exact parallax for stars in the solar neighborhood. Other methods to calculate the mass are considered to be indirect, they are not built on the law of gravity, but on the analysis of the stellar properties (luminosity, temperature, radius) which are somehow connected with the mass.

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Section: Data Processingmentioning

confidence: 86%

Section: History and Observationsmentioning

confidence: 99%

Estimating masses of selected stars in the Pulkovo program by means of astrometry methods

Shakht

Gorshanov

Vasilkova

2018

Res. Astron. Astrophys.

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“…The orbit was determined using the apparent motion parameters (AMP) method developed at Pulkovo for determining the elements of an orbit from a relatively short orbital arc [22,23]. The initial data for deriving the orbit of ADS 7251 are the five parameters of the apparent motion determined at the average time T 0 = 1986.698 for the observed arc of orbit.…”

Section: Determination Of the Orbitmentioning

confidence: 99%

Orbit determination and estimate of the component masses

et al. 2010

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Photographic observations of the visual binary star ADS 7251 were made from 1962 through 2006 on the 26-inch refractor at the Pulkovo Observatory. 206 plates were obtained and used to derive about 3000 relative positions. A uniform series of positions of the B-A components of ADS 7251 with errors in one annual average distance ρ and position angle θ of ±0".006 and ±0 o .02, respectively, have been used to determine the elements of the orbit and the sum of the masses of the components. The orbit has been determined using a method of apparent motion parameters developed at Pulkovo. The positions and motions of the components A and B relative to a system of reference stars have also been calculated from 146 of the plates; this made it possible to determine the position of the center of mass and the ratio of the masses of the components. The masses of A and B are 0.57 ¤ M and 0.53 ¤ M , respectively, a result that is consistent with their spectral classes and does not indicate the presence of significant excess mass.

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“…From 1970 to 2007, ADS 11061 was regularly observed photographically at Pulkovo. In 1996, the Pulkovo data were used for the first time to determine the family of orbits of the wide pair using the method of apparent motion parameters (AMP) developed by Kiselev at Pulkovo [3]. The orbital period of the system is estimated to exceed 50000 years and the eccentricity is close to unity, which means that this system is of great interest for further study.…”

Section: Introductionmentioning

confidence: 99%

Improved orbit for the visual-binary star 40/41 Dra

Afanasyeva

Grosheva

2012

Astrophysics

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Families of orbits of the visual binary star 40/41 Dra (ADS 11061), a near-polar visual binary star( m h J2000 00 18 = α ; 0 0 80 o J2000 ′ + = δ ) which is a wide pair in the neighborhood of the sun ( mas 19 = π t ), are calculated. Both components are spectrally binary and belong to the late spectral classes K2V and F7. The orbit was determined using a data base of photographic observations of this visual binary at the Pulkovo 26-inch refractor from 1970 through 2006. The latest spectroscopic data on the radial velocities and masses of the components are used in calculating the orbital elements. The family of orbits of 40/41 Dra was determined by the method of apparent motion parameters (AMP method) developed by Kiselev. The photographic plates were digitized and measured automatically for the first time. The parameters of the apparent motion were improved and the range of acceptable values for the true distances between the components was narrowed. The family of orbits was obtained by minimizing the O-C differences. The calculations are compared with the previously calculated family of orbits. The results of the measurements have been entered into the "Pulkovo Database of Observations of Visual Double Stars."

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Dynamical study of the wide visual binary ADS 12815 (16 Cyg)

Cited by 198 publications

References 2 publications

Estimating masses of selected stars in the Pulkovo program by means of astrometry methods

Estimating masses of selected stars in the Pulkovo program by means of astrometry methods

Orbit determination and estimate of the component masses

Improved orbit for the visual-binary star 40/41 Dra

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