Separated Fringe Packet Observations With the Chara Array. I. Methods and New Orbits for Χ Draconis, Hd 184467, and Hd 198084

Farrington, C.; Brummelaar, Theo A. ten; Mason, Brian D.; Hartkopf, William I.; McAlister, Harold A.; Raghavan, Deepak; Turner, N.; Sturmann, L.; Sturmann, J.; Ridgway, S. T.

doi:10.1088/0004-6256/139/6/2308

Cited by 37 publications

(29 citation statements)

References 18 publications

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“…And their positions on Girardi et al (2000a) The spectral types and luminosity classes of both components are assigned as K0V and K1.5V for the primary and secondary components respectively, and their positions on the evolutionary tracks are showed in Fig. 4, which are brighter than those given by Farrington et al (2010) as K2V and K4V.…”

Section: Resultsmentioning

confidence: 99%

Physical and geometrical parameters of CVBS X: the spectroscopic binary Gliese 762.1

Masda¹,

Al-Wardat

Neuhäuser³

et al. 2016

Res. Astron. Astrophys.

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We present the physical and geometrical parameters of the individual components of the close visual double-lined spectroscopic binary system Gliese 762.1, which were estimated using Al-Wardat's complex method for analyzing close visual binary systems. The estimated parameters of the individual components of the system are as follows: radius R A = 0.845 ± 0.09R ⊙ , R B = 0.795 ± 0.10R ⊙ , effective temperature T A eff = 5300 ± 50 K, T B eff = 5150 ± 50 K, surface gravity log g A = 4.52 ± 0.10, log g B = 4.54 ± 0.15 and luminosity L A = 0.51 ± 0.08L ⊙ , L B = 0.40 ± 0.07L ⊙ . New orbital elements are presented with a semi-major axis of 0.0865 ± 0.010 arcsec using the Hippracos parallax π = 58.96 ± 0.65 mas, and an accurate total mass and individual masses of the system are determined as M = 1.72 ± 0.60M ⊙ , M A = 0.89 ± 0.08M ⊙ and M B = 0.83 ± 0.07M ⊙ . Finally, the spectral types and luminosity classes of both components are assigned as K0V and K1.5V for the primary and secondary components respectively, and their positions on the H-R diagram and evolutionary tracks are given.

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Section: Resultsmentioning

confidence: 99%

Physical and geometrical parameters of CVBS X: the spectroscopic binary Gliese 762.1

Masda¹,

Al-Wardat

Neuhäuser³

et al. 2016

Res. Astron. Astrophys.

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“…We performed the adaptive grid search over a range of ±16 mas in ∆RA and ∆DEC using 0.1 mas steps and kept the solution with the lowest χ 2 as the global best-fit binary model. If the components in the binary are separated by more than the coherence length (∼ 8 mas for CLIMB measurements on 250−278 m baselines in the H-band), then they will begin to show two separated fringe packets in the interferometric scans (e.g., Farrington et al 2010Farrington et al , 2014. We selected a maximum search range of 16 mas, corresponding to twice the coherence length, to represent the separation at which the two fringe packets are completely separated and no longer overlap.…”

Section: Resolving the Long-period Binaries Wr 137 And Wr 138mentioning

confidence: 99%

The CHARA Array resolves the long-period Wolf–Rayet binaries WR 137 and WR 138

Richardson

Shenar

Roy-Loubier

et al. 2016

Mon. Not. R. Astron. Soc.

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We report on interferometric observations with the CHARA Array of two classical Wolf-Rayet stars in suspected binary systems, namely WR 137 and WR 138. In both cases, we resolve the component stars to be separated by a few milliarcseconds. The data were collected in the H-band, and provide a measure of the fractional flux for both stars in each system. We find that the WR star is the dominant H-band light source in both systems ( f WR,137 = 0.59 ± 0.04; f WR,138 = 0.67 ± 0.01), which is confirmed through both comparisons with estimated fundamental parameters for WR stars and O dwarfs, as well as through spectral modeling of each system. Our spectral modeling also provides fundamental parameters for the stars and winds in these systems. The results on WR 138 provide evidence that it is a binary system which may have gone through a previous mass-transfer episode to create the WR star. The separation and position of the stars in the WR 137 system together with previous results from the IOTA interferometer provides evidence that the binary is seen nearly edge-on. The possible edge-on orbit of WR 137 aligns well with the dust production site imaged by the Hubble Space Telescope during a previous periastron passage, showing that the dust production may be concentrated in the orbital plane.

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“…A1918b : Aitken (1918); Abt2006: Abt & Willmarth (2006); AST1999: Franz et al (1999); AST2001: Benedict et al (2001); B1960c: van den Bos (1960); Bag2005: Balega et al (2005); Baz1980b: Baize (1980); Chg1972: Chang (1972); CIA2010: Farrington et al (2010); Cou1960b: Couteau (1960; Doc1985c: Docobo & Costa (1985); Doc2008d: Docobo et al (2008); Doc2010d: Docobo & Ling (2010); Dom1978: Dommanget (1978; Dru1995: Drummond et al (1995); Duq1991b: Duquennoy et al (1991 Egg1956: Eggen (1956; Egn2008: Eggenberger et al (2008); Fek1983: Fekel & Tomkin (1983 FMR2008b: Rica Romero (2008 Frv1999: Forveille et al (1999; Gri1975: Griffin & Emerson (1975); Gri1998: Griffin (1998) Acknowledgements. We dedicate this paper to the memory of J. Dommanget, who initiated this study and could unfortunately not see it accomplished.…”

mentioning

confidence: 99%

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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Separated Fringe Packet Observations With the Chara Array. I. Methods and New Orbits for Χ Draconis, Hd 184467, and Hd 198084

Cited by 37 publications

References 18 publications

Physical and geometrical parameters of CVBS X: the spectroscopic binary Gliese 762.1

Physical and geometrical parameters of CVBS X: the spectroscopic binary Gliese 762.1

The CHARA Array resolves the long-period Wolf–Rayet binaries WR 137 and WR 138

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

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