Resolved double-lined spectroscopic binaries: A neglected source of hypothesis-free
parallaxes and stellar masses

Pourbaix, D.

doi:10.1051/aas:2000237

Cited by 146 publications

(119 citation statements)

References 22 publications

(32 reference statements)

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“…Our combined orbital solution using PHASES differential astrometry and previously published radial velocity measurements provides the best estimate of orbital parallax, at 54:39 AE 0:15 mas, in good agreement with the trigonometric values and the previous best orbital parallax of 55 AE 0:67 mas ( Pourbaix 2000). The orbital parallax determination is limited by the precision of the radial velocity measurements; simulations show that the high-precision radial velocity observations planned for the next observing season will improve the precision by a factor of 2.…”

Section: Parallaxsupporting

confidence: 83%

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PHASES High-Precision Differential Astrometry of δ Equulei

et al. 2005

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Delta Equulei is among the most well-studied nearby binary star systems. Results of its observation have been applied to a wide range of fundamental studies of binary systems and stellar astrophysics. It is widely used to calibrate and constrain theoretical models of the physics of stars. We report 27 high-precision differential astrometry measurements of Equ from the Palomar High-precision Astrometric Search for Exoplanet Systems (PHASES). The median size of the minor axes of the uncertainty ellipses for these measurements is 26 as. These data are combined with previously published radial velocity data and other previously published differential astrometry measurements using other techniques to produce a combined model for the system orbit. The distance to the system is determined to within one twentieth of a parsec, and the component masses are determined at the level of a percent. The constraints on masses and distance are limited by the precisions of the radial velocity data; we outline plans to improve this deficiency and discuss the outlook for further study of this binary.

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Section: Parallaxsupporting

confidence: 83%

“…Finally, a full three-dimensional model for the system was determined by Hans et al (1979). Since that time, several more orbital solutions have been offered (see, e.g., Starikova 1981; Duquennoy & Mayor 1988;Hartkopf et al 1996;Söderhjelm 1999;Pourbaix 2000).…”

Section: Orbital Modelsmentioning

confidence: 99%

PHASES High-Precision Differential Astrometry of δ Equulei

et al. 2005

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“…In Figure 6 we compare this relation with those obtained by using the data given by Pourbaix (2000) for 40 SB2s with known semimajor axes in AU and eccentricities ( log a 12 ¼ À1:2 þ 0:45e 12 þ 0:75e 2 12 ). We think that the coefficients of expression (2) are more accurate because our data set is bigger than Pourbaix's.…”

Section: Relation Between the Logarithm Of Minimum Semimajor Axis Andmentioning

confidence: 88%

“…3.-Distribution of the six visual-spectroscopic binaries in the i 12 -a 12 plane. Our results are indicated by a numbered square (according to numeration used in x 4.2), while those of previous works are indicated by the corresponding numbered triangle: 1 ( Docobo & Andrade 2006), 2 ( Hartkopf et al 1996), 3a ( Mason et al 1995), 3b ( Heintz 1996), 4a ( Forveille et al 1999), 4b ( Pourbaix 2000), 5 ( Tokovinin et al 2003), and 6 (Gatewood et al 2001). A diamond is used for the values given by Parsons (2004) (see x 4.2).…”

Section: New Orbits Of Visual Binariesmentioning

confidence: 99%

A Methodology for the Description of Multiple Stellar Systems with Spectroscopic Subcomponents

Docobo

Andrade

2006

ApJ

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We propose a methodology for analyzing triple stellar systems that include a visual double star wherein one of the components is a single-or double-lined spectroscopic binary. By using this methodology, we can calculate the most probable values of the spectroscopic binary's inclination, the angular separation between its components, and its stellar masses, and we can even estimate the spectral types. For a few W UMaYtype eclipsing binaries, stellar radii are also determined. Moreover, we present new formulae for calculating stellar masses depending on spectral type. In this way we have studied 61 triple systems, five of them W UMaYtype eclipsing binaries with low-mass subcomponents. In addition, we study nine quadruple systems, applying the same methodology and considering them twice as a triple system. With the aim of having more accurate orbital elements, we have taken advantage of the occasion to calculate and improve orbits. In this way we have used a new speckle measurement to improve the orbital elements for the binary Hu 506 AB. Also, new visual orbits are calculated for the binaries BAG 10 Aa and LAB 6 Aa. Finally, we give a list of five spectroscopic binaries with more than 0B1 for the maximum angular separation; these should be easily observable as visual binaries by means of interferometric techniques.

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“…The first reliable spectroscopic orbit was calculated by Griffin & Griffin (1982) and the first successful astrometric orbit was found from the observations obtained from the Hipparcos satellite (Soderhjelm 1999). Pourbaix (2000) combined the visual and spectroscopic observations of the components of the primary system into a single orbit solution. This approach allows the orbit to be computed with higher efficiency (Pourbaix & Eichhorn 1999).…”

Section: Cancrimentioning

confidence: 99%

Astrometric Studies of Aldebaran, Arcturus, Vega, the Hyades, and Other Regions

Gatewood

2008

The Astronomical Journal

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The results of astrometric studies in the regions of Groombridge 34A, the Hyades, Aldebaran, Ross 47, BD+5 • 1668, 81 Cancri, BD+15 • 2620, Arcturus, Vega, and Ross 248 are presented. Estimates of the absolute parallax of each star are presented and a mass estimate is present for 81 Cancri. Comments include the discussion of the apparent motions of a few previously suggested planetary systems.

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Resolved double-lined spectroscopic binaries: A neglected source of hypothesis-free parallaxes and stellar masses

Cited by 146 publications

References 22 publications

PHASES High-Precision Differential Astrometry of δ Equulei

PHASES High-Precision Differential Astrometry of δ Equulei

A Methodology for the Description of Multiple Stellar Systems with Spectroscopic Subcomponents

Astrometric Studies of Aldebaran, Arcturus, Vega, the Hyades, and Other Regions

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