Long-term monitoring of $\mathsf{\theta^1}$ Ori C: the spectroscopic orbit and an improved rotational period

Stahl, O.; Wade, G. A.; Petit, Véronique; Stober, B.; Schanne, L.

doi:10.1051/0004-6361:200809935

Cited by 35 publications

(52 citation statements)

References 27 publications

(47 reference statements)

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“…The orbital motion of the companion might also be responsible for the radial velocity variations reported by Stahl et al (1996Stahl et al ( , 2008 and others. Due to the incomplete coverage and the significant scatter in the derived velocities, it is not yet possible to derive the orbital elements of the spectroscopic orbit (Stahl et al 2008).…”

Section: Introductionmentioning

confidence: 80%

“…Besides the 15.424-day period which is associated with the wind from the primary, long-term radial velocity variations were also found (Vitrichenko 2002;Stahl et al 2008). Using a large data set covering more than 15 yrs of spectroscopic observations (plus three archival measurements, which extend the coverage to more than 64 yrs), Stahl et al (2008) showed that these variations are consistent with the orbital motion of a high-eccentricity binary system.…”

Section: Constraining the Binary Mass Ratiomentioning

confidence: 87%

“…Using a large data set covering more than 15 yrs of spectroscopic observations (plus three archival measurements, which extend the coverage to more than 64 yrs), Stahl et al (2008) showed that these variations are consistent with the orbital motion of a high-eccentricity binary system. Although the strong scatter within the radial velocity measurements prevents us from solving for the precise spectroscopic orbit, the combination of these data with our new orbital solution can be used to provide a first direct constraint on the mass ratio of the components in the θ 1 Ori C system.…”

Section: Constraining the Binary Mass Ratiomentioning

confidence: 94%

“…and it is known that these lines can show, with respect to each other, systematic velocity offsets on the order of 2-3 km s −1 (Stahl et al 2008), we used 3 km s −1 as minimum velocity error σ v i in order to avoid overweighting individual measurements. Table 3.…”

Section: Constraining the Binary Mass Ratiomentioning

confidence: 99%

“…Due to the incomplete coverage and the significant scatter in the derived velocities, it is not yet possible to derive the orbital elements of the spectroscopic orbit (Stahl et al 2008).…”

Section: Introductionmentioning

confidence: 99%

See 4 more Smart Citations

Tracing the young massive high-eccentricity binary system $\theta^{\mathsf 1}$Orionis C through periastron passage

Kraus¹,

Weigelt²,

Balega

et al. 2009

A&A

106

102

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Context. The nearby high-mass star binary system θ 1 Ori C is the brightest and most massive of the Trapezium OB stars at the core of the Orion Nebula Cluster, and it represents a perfect laboratory to determine the fundamental parameters of young hot stars and to constrain the distance of the Orion Trapezium Cluster. Aims. By tracing the orbital motion of the θ 1 Ori C components, we aim to refine the dynamical orbit of this important binary system. Methods. Between January 2007 and March 2008, we observed θ 1 Ori C with VLTI/AMBER near-infrared (H-and K-band) longbaseline interferometry, as well as with bispectrum speckle interferometry with the ESO 3.6 m and the BTA 6 m telescopes (Band V -band). Combining AMBER data taken with three different 3-telescope array configurations, we reconstructed the first VLTI/AMBER closure-phase aperture synthesis image, showing the θ 1 Ori C system with a resolution of ∼2 mas. To extract the astrometric data from our spectrally dispersed AMBER data, we employed a new algorithm, which fits the wavelength-differential visibility and closure phase modulations along the H-and K-band and is insensitive to calibration errors induced, for instance, by changing atmospheric conditions. Results. Our new astrometric measurements show that the companion has nearly completed one orbital revolution since its discovery in 1997. The derived orbital elements imply a short-period (P ≈ 11.3 yr) and high-eccentricity orbit (e ≈ 0.6) with periastron passage around 2002.6. The new orbit is consistent with recently published radial velocity measurements, from which we can also derive the first direct constraints on the mass ratio of the binary components. We employ various methods to derive the system mass (M system = 44 ± 7 M ) and the dynamical distance (d = 410 ± 20 pc), which is in remarkably good agreement with recently published trigonometric parallax measurements obtained with radio interferometry.

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Section: Introductionmentioning

confidence: 80%

Section: Constraining the Binary Mass Ratiomentioning

confidence: 87%

Section: Constraining the Binary Mass Ratiomentioning

confidence: 94%

Section: Constraining the Binary Mass Ratiomentioning

confidence: 99%

“…Due to the incomplete coverage and the significant scatter in the derived velocities, it is not yet possible to derive the orbital elements of the spectroscopic orbit (Stahl et al 2008).…”

Section: Introductionmentioning

confidence: 99%

See 3 more Smart Citations

Tracing the young massive high-eccentricity binary system $\theta^{\mathsf 1}$Orionis C through periastron passage

Kraus¹,

Weigelt²,

Balega

et al. 2009

A&A

106

102

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The kinematic characteristics of magnetic O‐type stars

2011

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Although magnetic fields have been discovered in ten massive O-type stars during the last years, the origin of their magnetic fields remains unknown. Among the magnetic O-type stars, two stars, HD36879 and HD57682, were identified as candidate runaway stars in the past, and theta^1 Ori C was reported to move rapidly away from its host cluster. We search for an explanation for the occurrence of magnetic fields in O-type stars by examining the assumption of their runaway status. We use the currently best available astrometric, spectroscopic, and photometric data to calculate the kinematical status of seven magnetic O-type stars with previously unknown space velocities. The results of the calculations of space velocities suggest that five out of the seven magnetic O-type stars can be considered as candidate runaway stars. Only two stars, HD155806 and HD164794, with the lowest space velocities, are likely members of Sco OB4 and NGC6530, respectively. However, the non-thermal radio emitter HD164794 is a binary system with colliding winds, for which the detected magnetic field has probably a different origin in comparison to other magnetic O-type stars.Comment: 5 pages, 2 tables, accepted for publication in Astronomische Nachrichte

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Characterizing the dynamical magnetosphere of the extremely slowly rotating magnetic O9.7 V star HD 54879 using rotational modulation of the Hα profile

Küker,

Järvinen,

Hubrig

et al. 2024

Astron Nachr

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The magnetic field in the O9.7 V star HD 54879 has been monitored for almost a decade. Spectropolarimetric observations reveal a rather strong mean longitudinal magnetic field that varies with a period of about 7.41 years. Observations in the H line show a variation with the same period, while the H line shows only little variation. Assuming the periodic variation to be caused by a slow rotation and a dipolar magnetic field, we find a magnetic field strength of 2 kG at the magnetic poles. With the relatively low mass loss rate of year−1, this star is a case of extremely strong magnetic confinement. Both theoretical arguments and numerical simulations indicate the presence of an extended disk of increased gas density in the equatorial plane of the magnetic field, where gas from the line‐driven stellar wind is trapped. This disk is likely to be the origin of the observed H emission, which peaks together with the strongest line‐of‐sight magnetic field. The profile of the H line is resolved in several components and shows a remarkable variability with the rotation period.

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Long-term monitoring of $\mathsf{\theta^1}$ Ori C: the spectroscopic orbit and an improved rotational period

Cited by 35 publications

References 27 publications

Tracing the young massive high-eccentricity binary system $\theta^{\mathsf 1}$Orionis C through periastron passage

Tracing the young massive high-eccentricity binary system $\theta^{\mathsf 1}$Orionis C through periastron passage

The kinematic characteristics of magnetic O‐type stars

Characterizing the dynamical magnetosphere of the extremely slowly rotating magnetic O9.7 V star HD 54879 using rotational modulation of the Hα profile

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