New orbits for two double stars eta Cassiopeiae and 36 Andromedae.

Baize, P.

doi:10.1086/105882

Cited by 6 publications

(8 citation statements)

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“…Observations of this system currently cover only about half an orbit, though the quality of its data set should improve greatly over the next few decades if, as expected, it passes through apastron during this period. For the time being, the present orbit is free from the systematic position angle errors of Baize's (1983) orbit, and is supported by observations made since its calculation in 1997. The mean radial velocities published for this binary are −12.95 ± 0.78 km s −1 (Tokovinin & Smekhov 2002) and −12.5 ± 0.3 km s −1 (Gontcharov 2006).…”

Section: Wds 10585+1711 a 2375 Ads 7997 Hip 53644 6th Cat Grade 4 supporting

confidence: 75%

Binary Stars With Components of Solar Type: 25 Orbits and System Masses

Docobo¹,

Ling²

2009

The Astronomical Journal

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FIN 359). In all of these systems, at least one component is of solar type. Total system masses were calculated in each case from the orbital period and semiaxis major together with the Hipparcos parallax, except in the cases for which there are no Hipparcos data or when these values are not precise. Other orbital and physical properties of these stars are also discussed. This paper is the second of three collating the revised double star orbits we have calculated in the past 15 yr.

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Section: Wds 10585+1711 a 2375 Ads 7997 Hip 53644 6th Cat Grade 4 supporting

confidence: 75%

Binary Stars With Components of Solar Type: 25 Orbits and System Masses

Docobo¹,

Ling²

2009

The Astronomical Journal

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“…Component C is distant and faint, so we ignored its flux. The AB system has a long period (≈ 462 y; Baize 1983), and we used the orbital elements from Baize (1983) to estimate the position of A,B. Balega & Balega (1988) and Baize (1993) determined an astrometric orbit for the close pair MCA 63 Aa,Ab that apparently consists of similar magnitude stars.…”

Section: Facilities: Chara Arraymentioning

confidence: 99%

A CHARA ARRAY SURVEY OF CIRCUMSTELLAR DISKS AROUND NEARBY Be-TYPE STARS

Touhami

Gies

Schaefer

et al. 2013

ApJ

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We report on a high angular resolution survey of circumstellar disks around 24 northern sky Be stars. The K-band continuum survey was made using the CHARA Array long baseline interferometer (baselines of 30 -331 m). The interferometric visibilities were corrected for the flux contribution of stellar companions in those cases where the Be star is a member of a known binary or multiple system. For those targets with good (u, v) coverage, we used a four-parameter Gaussian elliptical disk model to fit the visibilities and to determine the axial ratio, position angle, K-band photospheric flux contribution, and angular diameter of the disk's major axis. For the other targets with relatively limited (u, v) coverage, we constrained the axial ratio, inclination angle, and/or disk position

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“…In view of these results, we can conclude that although the classical Baize & Romani (1946) method shows a certain Similar conclusions are reached when considering Angelov's approach, using which neither parallaxes nor masses yield reliable values. These anomalies could be mainly due to the condition imposed in the series expansion given in Eq.…”

Section: Comparison With the Previous Modelsmentioning

confidence: 68%

“…Therefore, different sets of parameters (see Table 1) fitting a logarithmic linear MLR, such as that given in Eq. (1), have been considered in the past (see Baize & Romani 1946;McCluskey & Kondo 1972;Docobo & Andrade 2013), each of them derived from different data sources.…”

Section: A New Linear Mass-luminosity Relationmentioning

confidence: 99%

“…The pioneering works of Russell & Moore (1940) and Baize & Romani (1946) laid the foundation for the use of the massluminosity relation (MLR) along with Kepler's third law for calculating the dynamical parallax and the component masses of a main sequence (MS) visual binary. Although both approaches are equivalent, the Baize-Romani method has been more widely used over the years because of its simplicity and ease of use with different types of mass-luminosity arrays,…”

Section: Introductionmentioning

confidence: 99%

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Colour-dependent accurate modelling of dynamical parallaxes and masses of visual binaries

Andrade

2019

A&A

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Context. Two fundamental characteristics of binary systems are the masses of their components and their distance to the Earth. In this way, the dynamical parallax is an accurate and very helpful tool. Nevertheless, there has been some concern with regard to the use of a unique linear mass–luminosity relation (MLR) for the entire main sequence (MS). Aims. This article describes the accurate computation of both dynamical parallaxes and individual masses of visual binaries. The main aim is to formulate a model which would be suitable for binary systems attending to the exact locations of the components on the MS in the HR diagram. Methods. An analytical model was developed which allows calculation of dynamical parallaxes and individual masses using a non-linear MLR valid for the entire MS. This up-to-date MLR is given by a polynomial of degree 20. In contrast to previous approaches, this model can be applied even in the case of components with unequal masses, that is, with an arbitrarily large difference of magnitudes between them. On the other hand, considering the fundamental equation of the theory that forms the basis of the model, we propose to estimate uncertainties in parallax and masses using Monte Carlo simulations. Results. The model was validated by means of numerical tests using a synthetic sample comprising 103 systems. The results are much more accurate than those for previous models reported in the literature for deriving dynamical parallaxes and masses. Furthermore, we present dynamical parallaxes and individual masses for the 19 double-lined spectro-interferometric systems with definitive visual orbits and compare the former with the orbital parallaxes as well as with those measured by HIPPARCOS and Gaia. It is worth mentioning that the latter can only be a reliable source when the orbital motion is taken into account. Thus, at present, many Gaia DR2 parallaxes of binaries are biased. Conclusions. Our model, composed of an exact analytical theory, along with a non-linear MLR, guarantees high accuracy even in cases where the components are of unequal mass.

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New orbits for two double stars eta Cassiopeiae and 36 Andromedae.

Cited by 6 publications

References 0 publications

Binary Stars With Components of Solar Type: 25 Orbits and System Masses

Binary Stars With Components of Solar Type: 25 Orbits and System Masses

A CHARA ARRAY SURVEY OF CIRCUMSTELLAR DISKS AROUND NEARBY Be-TYPE STARS

Colour-dependent accurate modelling of dynamical parallaxes and masses of visual binaries

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