Analysis of periodic perturbations in the multiple system ADS 15571

Grosheva, E. A.

doi:10.1007/s10511-006-0039-6

Cited by 17 publications

(10 citation statements)

References 4 publications

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“…Observations from tahe nineteenth century were used for choosing the correct version of orbit (2) The ratio and sum of the masses of the components calculated using a dynamic analysis satisfy the "massluminosity" relationship for spectral class M0 and are consistent with the spectral class for main sequence stars. The error in the mass determination is less than 20%.…”

Section: Discussionmentioning

confidence: 99%

“…Many years of observations in this program have demonstrated our capabilities in discovering and confirming companions of this sort [2][3][4]. At the same time, our observational experience has made it possible to establish the limits and restrictions on the mass and discoverable period, which depend on the distance to a star, its mass, and the accuracy of the relative positions.…”

Section: Introductionmentioning

confidence: 96%

“…At the same time, our observational experience has made it possible to establish the limits and restrictions on the mass and discoverable period, which depend on the distance to a star, its mass, and the accuracy of the relative positions. A companion of the visual binary ADS 15571 with a most extended orbital period, about 23 years, has been detected by Grosheva [2] from a 40 year series of observations at Pulkovo. Here the lower limit for the mass of the companion was 0.6 ¤ M .…”

Section: Introductionmentioning

confidence: 97%

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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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Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 96%

Section: Introductionmentioning

confidence: 97%

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Orbit determination and estimate of the component masses

et al. 2010

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“…From these data, the AMP method is used to calculate the six major elements of the orbit (a, P, e, i, ω , Ω ) [10], where a is the major semiaxis of the orbit, P is the orbital period, e is the eccentricity, i is the inclination of the orbit, w is the argument of the pericenter, and Ω is the longitude of the rising node.…”

Section: The Methods Of Apparent Motion Parametersmentioning

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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“…Traditionally, to investigate the motions of the components of visual double stars, their observations are regularly carried out over decades (Izmailov et al (2010)). A careful analysis of the data series often leads to the detection of stars with invisible companions, also known as, astrometric binaries (Grosheva (2006)). For most nearby low-luminosity stars, we have no such dense, long, and homogeneous series of observations.…”

Section: Introductionmentioning

confidence: 99%

Δμ binaries among stars with large proper motions

Khovritchev¹,

Kulikova²

2015

Astron. Lett.

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Based on observations performed with the Pulkovo normal astrograph in 2008-2015 and data from sky surveys (DSS, 2MASS, SDSS DR12, WISE), we have investigated the motions of 1308 stars with proper motions larger than 300 mas/yr down to magnitude 17. The main idea of our search for binary stars based on this material is reduced to comparing the quasi-mean (POSS2-POSS1; an epoch difference of ≈50 yr) and quasi-instantaneous (2MASS, SDSS, WISE, Pulkovo; an epoch difference of ≈10 yr) proper motions. If the difference is statistically significant compared to the proper motion errors, then the object may be considered as a ∆µ-binary candidate. One hundred and twenty one stars from among those included in the observational program satisfy this requirement. Additional confirmations of binarity for a number of stars have been obtained by comparing the calculated proper motions with the data from several programs of stellar trigonometric parallax determinations and by analyzing the asymmetry of stellar images on sky-survey CCD frames. Analysis of the highly accurate SDSS photometric data for four stars (J0656+3827, J0838+3940, J1229+5332, J2330+4639) allows us to reach a conclusion about the probability that these ∆µ binaries are white dwarf + M dwarf pairs.

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Analysis of periodic perturbations in the multiple system ADS 15571

Cited by 17 publications

References 4 publications

Orbit determination and estimate of the component masses

Orbit determination and estimate of the component masses

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

Δμ binaries among stars with large proper motions

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