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We present the first visual orbit for the nitrogen-rich Wolf-Rayet binary, WR 133 (WN5o + O9I) based on observations made with the CHARA Array and the MIRC-X combiner. This orbit represents the first visual orbit for a WN star and only the third Wolf-Rayet star with a visual orbit. The orbit has a period of 112.8 d, a moderate eccentricity of 0.36,...
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Context 1
... scaling the uncertainties in the position, we added these values in quadrature for the major axis of the error ellipse (σ major ) and scaled the minor axis (σ minor ) to keep the axis ratio and position angle fixed according to the values derived from the covariance matrix. The results of the astrometric measurements are given in Table 2, with significant figures dependent on the individual measurements. In addition to the previously discussed parameters, we include the position angle of the error ellipse (σ PA ) in Table 2. Underhill & Hill (1994) found that the systemic velocities for the orbit of the Wolf-Rayet and O star components differed by about 100 km s −1 . ...Context 2
... results of the astrometric measurements are given in Table 2, with significant figures dependent on the individual measurements. In addition to the previously discussed parameters, we include the position angle of the error ellipse (σ PA ) in Table 2. Underhill & Hill (1994) found that the systemic velocities for the orbit of the Wolf-Rayet and O star components differed by about 100 km s −1 . ...Similar publications
Surface brightness-colour relations (SBCRs) are widely used for estimating angular diameters and deriving stellar properties. They are critical to derive extragalactic distances of early-type and late-type eclipsing binaries or, potentially, for extracting planetary parameters of late-type stars hosting planets. Various SBCRs have been implemented...
