The Secondaries of Solar‐Type Primaries. I. The Radial Velocities

Abt, Helmut A.; Willmarth, Daryl W.

doi:10.1086/498095

Cited by 44 publications

(98 citation statements)

References 38 publications

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“…• ± 3.1 • ) listed by Abt & Willmarth (2006) for the spectroscopic orbit (of A around the centre of mass of the system) is incorrect, as it should differ by 180…”

Section: Geometrical Elements System Coordinates Parallaxmentioning

confidence: 99%

“…Combining that orbit with earlier photocentric positions (Lippincott 1981;Russell & Gatewood 1984), masses could be derived: M A = 0.74 ± 0.06 M and M B = 0.17 ± 0.01 M . derived a preliminary spectroscopic orbit, and Abt & Willmarth (2006) obtained thereafter more radial velocities; however, Abt & Willmarth (2006) did not attempt to compute a combined orbit, and merged the orbital elements ofDuquennoy & Mayor (1991) and Drummond et al (1995). Because this is not fully satisfactory and is prone to confusion (as further discussed below), especially regarding the ambiguity on ω, we decided to compute a new combined orbit (Fig.…”

Section: Notesmentioning

confidence: 99%

“…WDS 01418+4237AB. Spectroscopic orbits were published by and Abt & Willmarth (2006). The present orbit (Table A.2) improves upon those, as it includes several unpublished CORAVEL velocities given in Table A.6.…”

Section: Geometrical Elements System Coordinates Parallaxmentioning

confidence: 99%

“…Based on available CORAVEL velocities (unpublished measurements are given in Table A.10), a combined astrometric/spectroscopic solution (Table A.2 and Fig. A.8) improves the spectroscopic orbital elements provided by Abt & Willmarth (2006) for that system. AC 15 AB is a triple system, with the separation Aa-Ab amounting to 0.228 and that of AB to 0.851 in 2005, according to Scardia et al (2008).…”

Section: Geometrical Elements System Coordinates Parallaxmentioning

confidence: 99%

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Are the orbital poles of binary stars in the solar neighbourhood anisotropically distributed?

Agati

Bonneau

Jorissen

et al. 2015

A&A

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We test whether or not the orbital poles of the systems in the solar neighbourhood are isotropically distributed on the celestial sphere. The problem is plagued by the ambiguity on the position of the ascending node. Of the 95 systems closer than 18 pc from the Sun with an orbit in the 6th Catalogue of Orbits of Visual Binaries, the pole ambiguity could be resolved for 51 systems using radial velocity collected in the literature and CORAVEL database or acquired with the HERMES/Mercator spectrograph. For several systems, we can correct the erroneous nodes in the 6th Catalogue of Orbits and obtain new combined spectroscopic/astrometric orbits for seven systems [WDS 01083+5455Aa,Ab; 01418+4237AB; 02278+0426AB (SB2); 09006+4147AB (SB2); 16413+3136AB; 17121+4540AB; 18070+3034AB]. We used of spherical statistics to test for possible anisotropy. After ordering the binary systems by increasing distance from the Sun, we computed the false-alarm probability for subsamples of increasing sizes, from N = 1 up to the full sample of 51 systems. Rayleigh-Watson and Beran tests deliver a false-alarm probability of 0.5% for the 20 systems closer than 8.1 pc. To evaluate the robustness of this conclusion, we used a jackknife approach, for which we repeated this procedure after removing one system at a time from the full sample. The false-alarm probability was then found to vary between 1.5% and 0.1%, depending on which system is removed. The reality of the deviation from isotropy can thus not be assessed with certainty at this stage, because only so few systems are available, despite our efforts to increase the sample. However, when considering the full sample of 51 systems, the concentration of poles toward the Galactic position l = 46.0• , b = 37• , as observed in the 8.1 pc sphere, totally vanishes (the Rayleigh-Watson false-alarm probability then rises to 18%).

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“…• ± 3.1 • ) listed by Abt & Willmarth (2006) for the spectroscopic orbit (of A around the centre of mass of the system) is incorrect, as it should differ by 180…”

Section: Geometrical Elements System Coordinates Parallaxmentioning

confidence: 99%

Section: Notesmentioning

confidence: 99%

Section: Geometrical Elements System Coordinates Parallaxmentioning

confidence: 99%

Section: Geometrical Elements System Coordinates Parallaxmentioning

confidence: 99%

See 2 more Smart Citations

Are the orbital poles of binary stars in the solar neighbourhood anisotropically distributed?

Agati

Bonneau

Jorissen

et al. 2015

A&A

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“…The system is also a single-lined spectroscopic binary (SB1), with an orbit published by Abt & Willmarth (2006). Orbital results for all five studies are given in Table 4.…”

Section: Gj 704 Abmentioning

confidence: 99%

Cool Subdwarf Investigations. Iii. Dynamical Masses of Low-Metallicity Subdwarfs

Jao¹,

Nelan²,

Henry³

et al. 2016

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We report dynamical mass measurements for the components of the previously known double-lined spectroscopic subdwarfs G 006-026 B and C using the Fine Guidance Sensors (FGS) on the Hubble Space Telescope. To build the empirical mass-luminosity relation for low metallicity subdwarfs, we collect four other subdwarf systems with dynamical masses that we compare to theoretical models for various metallicities on the mass-luminosity relation. For most stars, they fall in the regions where the models predict to be low metallicity. This effort highlights the scarcity of dynamical masses for subdwarfs and that much work remains to be done to improve the mass errors and metallicity measurements of low mass subdwarfs in our Galaxy.

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An Observational Review of Rotation in A Stars

Murphy

2014

Springer Theses

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The Secondaries of Solar‐Type Primaries. I. The Radial Velocities

Cited by 44 publications

References 38 publications

Are the orbital poles of binary stars in the solar neighbourhood anisotropically distributed?

Are the orbital poles of binary stars in the solar neighbourhood anisotropically distributed?

Cool Subdwarf Investigations. Iii. Dynamical Masses of Low-Metallicity Subdwarfs

An Observational Review of Rotation in A Stars

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