A coordinated X-ray and Optical Campaign of the Nearest Massive Eclipsing Binary, $\delta$ Orionis Aa: IV. A multiwavelength, non-LTE spectroscopic analysis

Abstract

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 $\delta$ 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 $\delta$ Ori lies at about twice the $Hipparcos$ distance, in the vicinity of the $\sigma$-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 $\Delta V\approx 2.{}^{\mathrm{m}}8$. The inferred parameters suggest the secondary is an early B-type dwarf ($\approx$ B1 V), while the tertiary is an early B-type subgiant ($\approx$ B0 IV). We find evidence for rapid turbulent velocities ($\sim 200$ km ${\mathrm{s}}^{-1}$) 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 ($\log L_{\text{X}}/L_{\text{Bol}}\approx -6.85$), initiating close to the stellar surface at $R_0\sim 1.1R_{\ast }$. Accounting for clumping, the mass-loss rate of the primary is found to be $\log \dot{M}\approx -6.4[M_{\odot }{\mathrm{yr}}^{-1}]$, which agrees with hydrodynamic predictions, and provides a consistent picture along the X-ray, UV, optical and radio spectral domains.

Accepted for Publication in APJ, 21 pages, 16 figures and 2 tables

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