First Visual Orbit for the Prototypical Colliding-Wind Binary Wr 140

Monnier, John D.; Zhao, M.; Pedretti, E.; Millan-Gabet, R.; Berger, J.‐P.; Traub, Wesley A.; Schloerb, F. Peter; Brummelaar, T. ten; McAlister, H. A.; Ridgway, Stephen T.; Sturmann, L.; Sturmann, J.; Turner, N.; Baron, Fabien; Kraus, Stefan; Tannirkulam, A.; Williams, P. M.

doi:10.1088/2041-8205/742/1/l1

Cited by 57 publications

(79 citation statements)

References 30 publications

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“…Table 3 lists the observation dates, the telescopes and calibrator stars used, the number of data points measured, and the average Fried parameter (r 0 ) for each night. Our data were reduced with the pipeline developed by J. D. Monnier, using the general method described in Monnier et al (2011) and extended to three beams (e.g., Kluska et al 2018), resulting in 4 https://www.gemini.edu/sciops/instruments/alopeke-zorro/ squared visibilities (V 2 ) for each baseline and closure phases (CP) for each closed triangle. Instrumental and atmospheric effects on the observed visibilities were measured using observations of stars with known angular diameters (HD 178207, 184170, 186760 and 187748) taken before and after the target.…”

Section: Climb Observationsmentioning

confidence: 99%

Visual Orbits of Spectroscopic Binaries with the CHARA Array. II. The Eclipsing Binary HD 185912

Lester¹,

Gies²,

Schaefer³

et al. 2019

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We present the visual orbit of the double-lined eclipsing binary, HD 185912, from long baseline interferometry with the CHARA Array. We also obtain echelle spectra from the Apache Point observatory to update the spectroscopic orbital solution and analyze new photometry from Burggraaff et al. to model the eclipses. By combining the spectroscopic and visual orbital solutions, we find component masses of M 1 = 1.361 ± 0.004 M ⊙ and M 2 = 1.331 ± 0.004 M ⊙ , and a distance of d = 40.75 ± 0.30 pc from orbital parallax. From the light curve solution, we find component radii of R 1 = 1.348 ± 0.016 R ⊙ and R 2 = 1.322 ± 0.016 R ⊙ . By comparing these observed parameters to stellar evolution models, we find that HD 185912 is a young system near the zero age main sequence with an estimated age of 500 Myr. 1 V1143 Cyg, HR 7484, HIP 96620; α = 19 : 38 : 41.183, δ = +54 : 58 : 25.642, V = 5.9 mag

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Section: Climb Observationsmentioning

confidence: 99%

Visual Orbits of Spectroscopic Binaries with the CHARA Array. II. The Eclipsing Binary HD 185912

Lester¹,

Gies²,

Schaefer³

et al. 2019

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“…Thus far, only two WR systems have been examined with interferometry. They are γ 2 Velorum (Hanbury Brown et al 1970, Millour et al 2007, North et al 2007) and WR 140 (Monnier et al 2004(Monnier et al , 2011. Both systems have well-defined doublelined spectroscopic orbits (Schmutz et al 1997, Fahed et al 2011) and consist of a carbon-rich WC star orbiting an O star.…”

Section: The Authorsmentioning

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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“…Others known are WR48a (Marchenko & Moffat 2007) and WR140 Williams et al 2009). The well-studied WR140 is the only one of these systems with kinematically measured masses, hosting a 15 M e WC7 star and a 36M e O5 star (Fahed et al 2011;Monnier et al 2011). The resolved mid-IR emission from WR112, which resembles a series of up to five successive broken shells and arc-like filaments, traces cooler dust and provides an opportunity to probe further into the mass-loss history of the central system.…”

Section: Introductionmentioning

confidence: 99%

Stagnant Shells in the Vicinity of the Dusty Wolf–Rayet–OB Binary WR 112

Lau

Hankins

Schödel

et al. 2017

ApJL

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We present high spatial resolution mid-infrared images of the nebula around the late-type carbon-rich Wolf-Rayet (WC)-OB binary system WR112 taken by the recently upgraded VLT spectrometer and imager for the midinfrared (VISIR) with the PAH1, Ne II_2, and Q3 filters. The observations reveal a morphology resembling a series of arc-like filaments and broken shells. Dust temperatures and masses are derived for each of the identified filamentary structures, which exhibit temperatures ranging from -+ 179 6 8 K at the exterior W2 filament to -+ 355 25 37 K in the central 3″. The total dust mass summed over the features is 2.6±0.4×10−5 M e . A multi-epoch analysis of mid-IR photometry of WR112 over the past ∼20 years reveals no significant variability in the observed dust temperature and mass. The morphology of the mid-IR dust emission from WR112 also exhibits no significant expansion from imaging data taken in 2001, 2007, and 2016, which disputes the current interpretation of the nebula as a high expansion velocity (∼1200 km s −1 ) "pinwheel"-shaped outflow driven by the central WC-OB collidingwind binary. An upper limit of 120 km s −1 is derived for the expansion velocity assuming a distance of 4.15kpc. The upper limit on the average total mass-loss rate from the central 3″ of WR112 is estimated to be. We leave its true nature as an open question, but propose that the WR112 nebula may have formed in the outflow during a previous red or yellow supergiant phase of the central Wolf-Rayet star.

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First Visual Orbit for the Prototypical Colliding-Wind Binary Wr 140

Cited by 57 publications

References 30 publications

Visual Orbits of Spectroscopic Binaries with the CHARA Array. II. The Eclipsing Binary HD 185912

Visual Orbits of Spectroscopic Binaries with the CHARA Array. II. The Eclipsing Binary HD 185912

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

Stagnant Shells in the Vicinity of the Dusty Wolf–Rayet–OB Binary WR 112

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