ICCD Speckle Observations of Binary Stars. XIX. An Astrometric/Spectroscopic Survey of O Stars

Mason, Brian D.; Gies, Douglas R.; Hartkopf, William I.; Bagnuolo, W. G.; Brummelaar, T. ten; McAlister, Harold A.

doi:10.1086/300234

Cited by 570 publications

(529 citation statements)

References 119 publications

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“…The eccentricity we find, , is larger than that in any of the known O star spece p 0.41 troscopic binaries with periods less than 6 days (see Fig. 3 of Mason et al 1998). The system probably obtained its large eccentricity during the supernova event that created the compact star (Nelemans, Tauris, & van den Heuvel 1999).…”

Section: Discussionmentioning

confidence: 50%

The Orbit of the Massive X-Ray Binary LS 5039

McSwain¹,

Gies²,

Riddle³

et al. 2001

The Astrophysical Journal

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We present the first spectroscopic orbit for the massive X-ray binary LS 5039, which we find to be a shortperiod ( days) and highly eccentric ( ) system. The low-mass function for P p 4.117 ‫ע‬ 0.011 e p 0.41 ‫ע‬ 0.05 the orbit appears to be most consistent with a neutron star companion, although a black hole remains a possibility if the system has a low inclination. The spectrum of the O7 V optical star appears to be normal for its type (suggesting that there is little flux in the red from an accretion disk) except that the C iv ll5801, 5812 lines are very weak, perhaps indicating the presence of CNO-processed gas in the O star. There is no evidence of Ha emission, so the system is probably not currently undergoing Roche lobe overflow. The projected rotational velocity, km s Ϫ1 , suggests that the optical star is rotating faster than synchronously with the V sin i p 131 ‫ע‬ 6 orbit. The peculiar component of the systemic radial velocity is Ϫ km s Ϫ1 , so the system is not a runaway 17 ‫ע‬ 3 star (at least not in this dimension).

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Section: Discussionmentioning

confidence: 50%

The Orbit of the Massive X-Ray Binary LS 5039

McSwain¹,

Gies²,

Riddle³

et al. 2001

The Astrophysical Journal

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“…Radial velocities of this binary (16 Sgr, O9.5 II-III, V = 5.98) were published by Feast et al (1955), Garmany et al (1980) (Mason et al 1998). A preliminary value for the magnitude difference between the two components was 2 mag.…”

Section: Hd 167263mentioning

confidence: 98%

“…In particular, binaries offer the opportunity to provide precise absolute stellar quantities (masses, radii, and luminosities) for challenging theoretical predictions. Listings of O-type stars such as those by Mason et al (1998) and Maíz-Apellániz et al (2004) contain many early-type objects, for which their status as single or double stars -either SB1 or SB2 -is still uncertain. Recently, Chini et al (2012) presented an extensive spectroscopic survey of OB stars regarding their binarity, which was based on several thousand spectra obtained with the ESO FEROS and Bochum University BESO echelle spectrographs over the past years.…”

Section: Introductionmentioning

confidence: 99%

New and revised parameters for several southern OB binaries

Mayer

Drechsel

Irrgang

2014

A&A

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Using ESO FEROS archive spectra of several southern OB-type binaries, we derived periods for three SB2 spectroscopic binaries, HD 97166, HD 115455, and HD 123590, and two SB1 systems, HD 130298 and HD 163892. It was also possible to use new FEROS spectra to improve the parameters of the known binaries, KX Vel and HD 167263. For KX Vel, we determined a dynamic mass of the primary of 16.8 M , while the evolutionary model suggests a higher value of 20.2 M . We derived an improved period for HD 167263, and in its spectra, we recognized contributions of both of its interferometric components.

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“…The binary frequency is about 50% for low-mass stars (see Duquennoy & Mayor 1991;Fischer & Marcy 1992) and seems to be significantly higher (>70%) for the more massive O-and B-type stars (see Mason et al 1998;Abt et al 1990;Preibisch et al 1999;. The high multiplicity of massive stars, and in particular the large number of very close systems (see e.g.…”

Section: Introductionmentioning

confidence: 99%

Orbital motion of the massive multiple stars in the Orion Trapezium

Schertl

Balega

Preibisch

et al. 2003

A&A

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Abstract. We present bispectrum speckle interferometry of the multiple Orion Trapezium stars θ 1 Ori A, θ 1 Ori B, and θ 1 Ori C obtained with the SAO 6 m telescope in Russia over a period of 5.5 years (epochs 1995-2001). Our diffraction-limited images have a resolution λ/D of 42 mas (J-band), 57 mas (H-band) and 76 mas (K-band). We clearly detect motion of the companions relative to their primary stars in the systems θ 1 Ori A1-2 (mean separation ρ ∼ 220 mas, change in position angle ∆PA = 6 • ), θ 1 Ori B2-3 (ρ ∼ 205 mas, ∆PA = 8 • ), and θ 1 Ori C1-2 (ρ ∼ 37 mas, ∆PA = 18 • ). In our K-band image of θ 1 Ori B we resolve a fourth visual component, confirming its discovery by Simon et al. (1999). We determine the J, H, and K magnitudes of the system components and estimate the stellar masses of the companions in the HR-diagram. The companions θ 1 Ori C2 and θ 1 Ori B2 show clear evidence of near-infrared excess in the color-color diagram. The companions θ 1 Ori A2 and θ 1 Ori B3 show much stronger extinction than their primary stars, providing evidence of the presence of circumstellar material around the companions.

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ICCD Speckle Observations of Binary Stars. XIX. An Astrometric/Spectroscopic Survey of O Stars

Cited by 570 publications

References 119 publications

The Orbit of the Massive X-Ray Binary LS 5039

The Orbit of the Massive X-Ray Binary LS 5039

New and revised parameters for several southern OB binaries

Orbital motion of the massive multiple stars in the Orion Trapezium

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