Statistical study of visual binaries

Верещагин, С. В.; Kraicheva, Z.; Popova, E. I.; Тутуков, А. В.; Yungelson, L. R.

doi:10.1007/bf00656217

Cited by 23 publications

(19 citation statements)

References 4 publications

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“…The ovb only contains information about the semi-major axis a = a 1 +a 2 of the relative orbit of the components around each other. For the majority of visual binaries, both from the ovb and the wds, authors have to resort to a mass-luminosity relation (Trimble and Walker 1986), or a spectral-type-mass relation (Vereshchagin et al 1988) to determine masses and mass-ratios. The major selection effect for visual binaries is the magnitude difference of the components with respect to their angular separation.…”

Section: Visual Binary Parametersmentioning

confidence: 99%

“…The semi-major axis a, of the relative orbit of binary systems, is assumed to be distributed proportional to 1/a, according to Vereshchagin et al (1987Vereshchagin et al ( , 1988. Values of a were generated in the range 1.4R Roche < a < 10 6 R .…”

Section: Distributions Of Generated Parametersmentioning

confidence: 99%

“…One such restriction is a maximum magnitude for the systems considered. Vereshchagin et al (1987Vereshchagin et al ( , 1988 consider the sample of systems in the wds with primary magnitudes m prim < 7 m the most complete and unbiased one. Therefore, systems with primaries fainter than 7 m are also rejected in the selection effects simulation programme.…”

Section: Maximum Primary Magnitudementioning

confidence: 99%

“…Modern statistical data for parameters of visual binary stars have been presented by Vereshchagin et al (1987Vereshchagin et al ( , 1988, Poveda et al (1982), Trimble and Walker (1986) and Kraicheva et al (1985). Vereshchagin et al and Poveda et al derived their data from the Index Catalogue of Visual Double Stars (ids) by Jeffers, Van den Bos and Greeby (1963), a predecessor of the The Washington Double Star Catalogue (wds) by Worley and Douglass 1 (1984).…”

Section: Introductionmentioning

confidence: 99%

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The mass-ratio distribution of Visual Binary Stars

Hogeveen

1990

Astrophys Space Sci

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The selection effects that govern the observations of Visual Binary Stars are investigated, in order to obtain a realistic statistical distribution of the mass-ratio q = M sec /M prim . To this end a numerical simulation programme has been developed, which 'generates' binary stars and 'looks' at them to determine whether an observer on Earth would be able to detect them. The simulations show that for mass-ratios q > 0.35, observations are expected to reveal the real q-distribution, while for massratios q < 0.35 selection effects begin to play a major part. It is found that the observed mass-ratio distribution for main-sequence systems, derived from the Index Catalogue of Visual Binary Stars (ids), can be explained by a distribution of secondary masses according to the Initial Mass Function (imf), i.e. φ(M) ∝ M −2.7 . From the Fourth Catalogue of Orbits of Visual Binary Stars (ovb) authors find a q-distribution that peaks strongly for q-values close to q = 1. It is shown that this mass-ratio distribution may be the result of a sampling selection effect. Due to this sampling selection effect, the ovb is a considerably more biased sample of the binary population in our Galaxy than the ids. Numerical simulations of biased sampling show that the q-distribution, found from the ovb, is not incompatible with the distribution of secondary masses according to the imf (for q > 0.35), found from the ids.Because of the selection effects, it is difficult to establish the real q-distribution for q < 0.35. If the real q-distribution departs from φ(q) ∝ q −2.7 for q ≤ 0.35, about 36% of all stars are in visual binaries (i.e. if the q-distribution is assumed to be flat for 0 < q < 0.35); if the distribution flattens for q ≤ 0.25, about 60% of the stars must be primaries of visual binaries.

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Section: Visual Binary Parametersmentioning

confidence: 99%

Section: Distributions Of Generated Parametersmentioning

confidence: 99%

Section: Maximum Primary Magnitudementioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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The mass-ratio distribution of Visual Binary Stars

Hogeveen

1990

Astrophys Space Sci

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“…To calculate the rate of these captures, we assumeÖpik's Law (Öpik 1924), a flat distribution of binary semimajor axes a in units of log(a), between a min and a max . Following Vereshchagin et al (1988) and Kouwenhoven et al (2007) we adopt a min = 5R and a max = 5 × 10 6 R . We only consider captures with r max < r t,c , with the cloud's tidal radius conservatively given by r t,c = r infl .…”

Section: Interactions With the Bound Cloudmentioning

confidence: 99%