A COORDINATED X-RAY AND OPTICAL CAMPAIGN OF THE NEAREST MASSIVE ECLIPSING BINARY, δ ORIONIS Aa. I. OVERVIEW OF THE X-RAY SPECTRUM

@article{Corcoran2015ACX,
  title={A COORDINATED X-RAY AND OPTICAL CAMPAIGN OF THE NEAREST MASSIVE ECLIPSING BINARY, $\delta$ ORIONIS Aa. I. OVERVIEW OF THE X-RAY SPECTRUM},
  author={Michael F. Corcoran and Joy S. Nichols and Herbert Pablo and Tomer Shenar and Andrew M. T. Pollock and Wayne Lee Waldron and Anthony F. J. Moffat and Noel D. Richardson and Christopher M. P. Russell and Kenji Hamaguchi and David P. Huenemoerder and Lidia M Oskinova and W. R. Hamann and Ya{\"e}l Naz{\'e} and Richard Ignace and Nancy Remage Evans and Jamie R. Lomax and Jennifer L. Hoffman and Kenneth Gayley and Stanley P. Owocki and Maurice A. Leutenegger and Theodore R. Gull and Karen Tabetha Hole and J. Lauer and Rosina C. Iping},
  journal={The Astrophysical Journal},
  year={2015},
  volume={809}
}
We present an overview of four deep phase-constrained Chandra HETGS X-ray observations of δ Ori A. Delta Ori A is actually a triple system that includes the nearest massive eclipsing spectroscopic binary, δ Ori Aa, the only such object that can be observed with little phase-smearing with the Chandra gratings. Since the fainter star, δ Ori Aa2, has a much lower X-ray luminosity than the brighter primary (δ Ori Aa1), δ Ori Aa provides a unique system with which to test the spatial distribution of… 
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We present time-resolved and phase-resolved variability studies of an extensive X-ray high-resolution spectral data set of the δ Ori Aa binary system. The four observations, obtained with Chandra
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Improved model of Delta Orionis
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References

SHOWING 1-10 OF 61 REFERENCES
A COORDINATED X-RAY AND OPTICAL CAMPAIGN OF THE NEAREST MASSIVE ECLIPSING BINARY, δ ORIONIS Aa. II. X-RAY VARIABILITY
We present time-resolved and phase-resolved variability studies of an extensive X-ray high-resolution spectral data set of the δ Ori Aa binary system. The four observations, obtained with Chandra
A Coordinated X-Ray and Optical Campaign of the Nearest Massive Eclipsing Binary, δ Orionis Aa. IV. A Multiwavelength, Non-LTE Spectroscopic Analysis
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
A COORDINATED X-RAY AND OPTICAL CAMPAIGN OF THE NEAREST MASSIVE ECLIPSING BINARY, δ ORIONIS Aa. III. ANALYSIS OF OPTICAL PHOTOMETRIC (MOST) AND SPECTROSCOPIC (GROUND-BASED) VARIATIONS
We report on both high-precision photometry from the Microvariability and Oscillations of Stars (MOST) space telescope and ground-based spectroscopy of the triple system δ Ori A, consisting of a
High-resolution X-ray spectroscopy of bright O-type stars
Archival X-ray spectra of the four prominent single, non-magnetic O stars ζ Pup, ζ Ori, ξ Per, ζ Oph, obtained in high resolution with Chandra HETGS/MEG have been studied. The resolved X-ray emission
An Extensive Collection of Stellar Wind X-Ray Source Region Emission Line Parameters, Temperatures, Velocities, and Their Radial Distributions as Obtained from Chandra Observations of 17 OB Stars
Chandra high energy resolution observations have now been obtained from numerous nonpeculiar O and early B stars. The observed X-ray emission line properties differ from prelaunch predictions, and
THE CORRELATION BETWEEN X-RAY LINE IONIZATION AND OPTICAL SPECTRAL TYPES OF THE OB STARS
Marked correlations are reported between the ionization of the X-ray line spectra of normal OB stars, as observed by the Chandra X-Ray Observatory, and their optical spectral types. These
X-ray spectra of Orion OB supergiants
The spectra are at a higher energy resolution than earlier X-ray observations of OB supergiants, and this allows stronger constraints to be placed on the location of the emission source in the outer
The X-ray spectrum of δ Orionis observed by LETGS aboard Chandra
Aims. We analyze the high-resolution X-ray spectrum of the supergiant O-star δ Orionis (O9.5II) with line ratios of He-like ions and a thermal plasma model, and we examine its variability. Methods.
Physical elements of the eclipsing binary δ Orionis
For years, δ Orionis was considered a normal binary with an 09.5 II primary exhibiting apsidal-line advance. However, radial-velocity curves of both binary components have been derived from the IUE
The Einstein X-ray Observatory Catalog of O-type stars
A catalog of X-ray count rates for all O-type stars surveyed by the Einstein Observatory is presented. The procedures by which the IPC and High Resolution Imager rates are converted to emitted X-ray
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