Improved Orbit and Mass of the Binary Star 61 Cyg Based on Photographic Observations at Pulkovo

Shakht, N. A.; Gorshanov, D. L.; Vasilkova, O. O.

doi:10.1007/s10511-017-9502-9

Cited by 5 publications

(2 citation statements)

References 10 publications

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“…Now we reexamine our results with an additional series of observations during 1997-2006. Two variants of orbits, obtained using parallax 0.2861 ′′ ± 0.0005 ′′ from the RECONS.org website, are given in Shakht et al (2017). (http://www.recons.org/TOP100.posted.htm, from the REsearch Consortium On Nearby Stars (RECONS)).…”

Section: Data Processingmentioning

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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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: 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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“…Обозначения приведены в тексте. В последней колонке дана ссылка на статью, в которой получена эта орбита ([0] -если в настоящей работе; [1]= (Кияева et al, 2017); [2]= (Кияева et al, 2020); [3]= (Кияева et al, 2001); [4]= (Романенко, Измайлов, 2021); [5]= (Кияева, Измайлов, 2018); [6]= (Shakht et al, 2007); [7]= (Кияева, Романенко, 2020); [8]= (Shakht et al, 2020); [9]= (Романенко, Киселев, 2014); [10]= (Романенко, 2018); [11]=(Грошева, 2006); [12]=(Киселев et al, 2000); [13]=(Киселев et al, 2009); [14]=(Романенко, 2017);[15]=(Кияева, Горыня, 2015); [16]=(Shakht et al, 2017); [17]=(Grosheva, 2006); [18] = (Kiyaeva et al, 2021)). doi: 10.31725/0367-7966-2022-227-11 Известия Главной Астрономической Обсерватории в Пулкове, № 227…”

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

Kiyaeva¹,

Izmailov²,

Shakht³

et al. 2022

Publ. Pulk. Obs.

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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 orbit determination method uses 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, part of them recalculated, new orbits added. For the stars of Pulkovo program of observations with a 26-inch refractor, the data from the Gaia DR2 catalog were analised. The orbits of 16 stars were calculated on these data. The direction of the motion derived from Gaia DR2 at the instant 2015.5 contradicts to the series of all observations for 20 stars. The probable reason is in the presence of inner subsystems. The orientation of the obtained orbits in the Galaxy frame is also given.

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Study of Brightness Variability of the Components of the Visual Binary System 61 Cyg Based on Observations at the Normal Astrograph of the Pulkovo Observatory

Polyakov

Vasilkova²,

Gorshanov

et al. 2018

Astrophysics

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Improved Orbit and Mass of the Binary Star 61 Cyg Based on Photographic Observations at Pulkovo

Cited by 5 publications

References 10 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

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

Study of Brightness Variability of the Components of the Visual Binary System 61 Cyg Based on Observations at the Normal Astrograph of the Pulkovo Observatory

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