The supermassive black hole at the center of our galaxy: Determination of its main physical parameters

Kisselev, A. A.; Gnedin, Yu. N.; Grosheva, E. A.; Shakht, N. A.; Gorshanov, D. L.; Piotrovich, M. Yu.

doi:10.1134/s1063772907020047

Cited by 3 publications

(2 citation statements)

References 36 publications

(53 reference statements)

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“…The detailed algorithms have been published in [3]. The method has been developed also for determination of the asteroids and double stars orbits [4], and for a special case of star rotating around the blackhole in the center of our Galaxy [5].…”

Section: B Amp-methodsmentioning

confidence: 99%

Study of the Solar system with the EPOS-software and Orbital Stellar Stereoscopic Observatory

Shakht

Kiselev²,

L'Vov³

et al. 2011

2011 2nd International Conference on Space Technology

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In the Pulkovo observatory the observations of the Solar system objects and improvement of the processing methods are performing. EPOS (Ephemeris Program for Objects of the Solar system) is the effective math-soft application for study and ephemeris support of observations of such objects. There are the options in EPOS for calculation of the orbits of asteroids including NEAs and using the observations at the relatively short arc.Also we would like to present shortly our method of Apparent Motion Parameters (AMP) for determinations of orbits of artificial satellites and other objects from observations of short arc. The research program of the Orbital Stellar Stereoscopic Observatory (OSSO) is based on the stereoscopic method of observation for fundamental studies in the area of Celestial Mechanics, Asteroid and Comet Impact Hazard, Stellar Astronomy,Astrometry and Astrophysics with the magnitude of the target objects ranging from 8 m to 25 m . This project is designing for stellar-like objects observations, including the main types of the Solar system bodies.

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Section: B Amp-methodsmentioning

confidence: 99%

Study of the Solar system with the EPOS-software and Orbital Stellar Stereoscopic Observatory

Shakht

Kiselev²,

L'Vov³

et al. 2011

2011 2nd International Conference on Space Technology

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“…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%

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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Checking the possibility of determining the relative orbits of stars rotating around the center body of the Galaxy

2022

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The results of observations of selected stars orbiting the central body of our Galaxy, which, according to the latest data, has a mass of about 4 million of solar mass, are considered. Using the methods of observation and processing of binary stars used at the Pulkovo Observatory and the published exact relative positions of the star-central body obtained with the Keck and VLT telescopes, we checked the possibility of determining the preliminary orbits of the above objects in some cases from observations covering sufficient short arc in relation to the turnover period. Examples are the stars S02 and S102 with published positions and the graphical data for S27 and S4711. We attempted to calculate the assumed relativistic effects in accordance with the orbital elements obtained by Pulkovo methods. In this case, the estimates of the O–C errors for these orbits turned out to be comparable with the O–C errors for the orbits published by the Keck and VLT observers, in some cases about several milliarcseconds. The theoretical relativistic parameters also turned out to be of the same order of value with the results of these authors.

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The supermassive black hole at the center of our galaxy: Determination of its main physical parameters

Cited by 3 publications

References 36 publications

Study of the Solar system with the EPOS-software and Orbital Stellar Stereoscopic Observatory

Study of the Solar system with the EPOS-software and Orbital Stellar Stereoscopic Observatory

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

Checking the possibility of determining the relative orbits of stars rotating around the center body of the Galaxy

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