The Orbits of 451 Wide Visual Double Stars

Izmailov, I. S.

doi:10.1134/s106377371901002x

Cited by 34 publications

(22 citation statements)

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“…The eccentricity, e = 0.915 +0.020 −0.018 , is found to be less extreme than the latest reported value of 0.979 ± 0.011 by Izmailov (2019). 7 Our semimajor axis is some-…”

Section: Analysis and Resultscontrasting

confidence: 55%

“…what smaller compared to the estimates by both Baize (1980) and Izmailov (2019), but larger than that of Peterson & Solensky (1988). Our adopted model is shown in Figure 1 along with the observations, with the orbit by Izmailov (2019) added for reference (see footnote 7).…”

Section: · · ·mentioning

confidence: 85%

“…However, that orbit no longer matches the more recent data. A revised model was proposed by Peterson & Solensky (1988) that is more eccentric (e = 0.901 ± 0.027), and a more recent one by Izmailov (2019) increases the eccentricity even further to 0.979 ± 0.011.…”

Section: Visual Measurementsmentioning

confidence: 99%

“…The adopted weights for the second solution resulted from a complicated procedure that is not entirely clear to the present author, apparently involving an assessment of measurement residuals from different sources and also from other binaries, although no specific details were given for 80 Tau. The solution favored by Izmailov (2019) is the one that uses different weights, which gives the eccentricity we reported. In the other solution the eccentricity is slightly smaller (e = 0.925 ± 0.019).…”

Section: · · ·mentioning

confidence: 99%

“…Observations of 80 Tau along with our adopted model from Table 3. The dashed line represents the orbit by Izmailov (2019). Also shown in the top panel are the dates of the observations that did not resolve the binary (triangles).…”

Section: · · ·mentioning

confidence: 99%

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Dynamical Masses for the Hyades Binary 80 Tauri

Torres

2019

ApJ

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The empirical mass-luminosity relation in the Hyades cluster rests on dynamical mass determinations for five binary systems, of which one is eclipsing and the other four are visual or interferometric binaries. The last one was identified and first measured more than 20 years ago. Here we present dynamical mass measurements for a new binary system in the cluster, 80 Tau, which is also a visual system with a much longer orbital period of about 170 yr. Although we lack the radial-velocity information that has enabled the individual mass determinations in all of the previous binaries, we show that it is still possible to derive the component masses for 80 Tau using only astrometric observations. This is enabled by the accurate proper motion measurements from the Hipparcos and Gaia missions, which constrain the orbital acceleration in the plane of the sky. Separate proper motion values from Gaia for the primary and secondary provide a direct constraint on the mass ratio. Our mass measurements, M A = 1.63 +0.30 −0.13 M ⊙ and M B = 1.11 +0.21 −0.14 M ⊙ , are consistent with the mass-luminosity relation defined by the five previously known systems, which in turn is in good agreement with current models of stellar evolution.

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“…The eccentricity, e = 0.915 +0.020 −0.018 , is found to be less extreme than the latest reported value of 0.979 ± 0.011 by Izmailov (2019). 7 Our semimajor axis is some-…”

Section: Analysis and Resultscontrasting

confidence: 55%

Section: · · ·mentioning

confidence: 85%

Section: Visual Measurementsmentioning

confidence: 99%

Section: · · ·mentioning

confidence: 99%

Section: · · ·mentioning

confidence: 99%

See 3 more Smart Citations

Dynamical Masses for the Hyades Binary 80 Tauri

Torres

2019

ApJ

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Astrometric observations of visual binaries using 26‐inch refractor at Pulkovo Observatory during 2014–2019

2020

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We present 18,365 astrometric observations of 290 visual binaries obtained with the 26‐inch refractor of Pulkovo Observatory during 2014–2019. The separation between components is from 1″.3 to 37″ with a median value of 4″.8. For a single observation, the mean separation error is 0″.013, and the mean position angle error is 0∘.44/ρ, where ρ is an angular distance in arcseconds. We compare the observations of sample stars with the data from the Gaia DR2 catalog and the results of the ground‐based observations performed with other telescopes.

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Orbital Elements of visual binary stars with very short arcs: With application to double stars from the 1829 southern double star catalog of James Dunlop

2022

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Binary double stars are those whose binding energies are less than zero. Obtaining binary star orbits from short arcs has been a long-standing problem in astrophysics. A method is presented and tested here, which addresses the problem by using space-based astrometry, photometry, and astrophysical data, together with historic measures, to generate and constrain a range of possible first-order Grade 5 orbits. After testing the method on an established binary star, we apply the method to eight double stars from the first published catalog of southern double stars, that of Dunlop (1829) and generate orbits for five. The mean orbital period is ∼81,000 years, and the mean semi-major axis is ∼76 ′′ with a typical uncertainty of the Orbital Elements of ∼37%. Their Orbital Elements and associated plots are also presented.

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The Orbits of 451 Wide Visual Double Stars

Cited by 34 publications

References 10 publications

Dynamical Masses for the Hyades Binary 80 Tauri

Dynamical Masses for the Hyades Binary 80 Tauri

Astrometric observations of visual binaries using 26‐inch refractor at Pulkovo Observatory during 2014–2019

Orbital Elements of visual binary stars with very short arcs: With application to double stars from the 1829 southern double star catalog of James Dunlop

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