A COORDINATED X-RAY AND OPTICAL CAMPAIGN OF THE NEAREST MASSIVE ECLIPSING BINARY, δ ORIONIS Aa. IV. A MULTIWAVELENGTH, NON-LTE SPECTROSCOPIC ANALYSIS

• Main Authors: Shenar, T. (Author), Oskinova, Lidia M. (Author), Hamann, W.-R (Author), Corcoran, M. F. (Author), Moffat, A. F. J. (Author), Pablo, H. (Author), Richardson, N. D. (Author), Waldron, W. L. (Author), Nichols, Joy S. (Author), Todt, H. (Author), Hoffman, J. L. (Author), Pollock, A. M. T. (Author), Negueruela, I. (Author), Huenemoerder, David P. (Contributor), Maiz Apellaniz, J. (Author), Naze, Y. (Author)
• Other Authors: MIT Kavli Institute for Astrophysics and Space Research (Contributor)
• Format: Article
• Language: English
• Published: IOP Publishing, 2015-11-24T20:29:36Z.
• Subjects: Article
• Online Access: Get fulltext

 Eclipsing systems of massive stars allow one to explore the properties of their components in great detail. We perform a multi-wavelength, non-LTE analysis of the three components of the massive multiple system δ Ori A, focusing on the fundamental stellar properties, stellar winds, and X-ray characteristics of the system. The primary's distance-independent parameters turn out to be characteristic for its spectral type (O9.5 II), but usage of the Hipparcos parallax yields surprisingly low values for the mass, radius, and luminosity. Consistent values follow only if δ Ori lies at about twice the Hipparcos distance, in the vicinity of the σ-Orionis cluster. The primary and tertiary dominate the spectrum and leave the secondary only marginally detectable. We estimate the V-band magnitude difference between primary and secondary to be ∆V ≈ 2[m over .]8. The inferred parameters suggest that the secondary is an early B-type dwarf (≈B1 V), while the tertiary is an early B-type subgiant (≈B0 IV). We find evidence for rapid turbulent velocities (~200 km s[superscript −1]) and wind inhomogeneities, partially optically thick, in the primary's wind. The bulk of the X-ray emission likely emerges from the primary's stellar wind (log L[subscript X]/L[subscript Bol] ≈ -6.85), initiating close to the stellar surface at R[subscript 0] ~ 1.1 R[subscript *]. Accounting for clumping, the mass-loss rate of the primary is found to be log [. over dot] ≈ -6.4 (M[subscript ʘ] yr[superscript -1]), which agrees with hydrodynamic predictions, and provides a consistent picture along the X-ray, UV, optical, and radio spectral domains.