A study of the radial velocity of the star Θ1 Ori C

Vitrichenko, E. A.

doi:10.1134/1.1476981

Cited by 18 publications

(30 citation statements)

References 12 publications

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“…Finally, although the findings of Vitrichenko (2002) differ clearly from those of Donati et al (2002), our present data are unable to discriminate between them.…”

Section: Spectroscopic Results For the θ 1 Ori C Systemcontrasting

confidence: 51%

“…This period suggests a semimajor axis of a ∼ 1 AU, and therefore, the spectroscopic companion cannot be the speckle companion. However, Vitrichenko (2002) also claimed evidence for long-term variations of the mean radial velocity of the θ 1 Ori C spectroscopic system, which he interpreted as an indication of the presence of a third component. For this third component he derived a period of 120 yr, suggesting a semimajor axis of a ∼ 80 AU.…”

Section: Spectroscopic Results For the θ 1 Ori C Systemmentioning

confidence: 99%

“…Donati et al (2002) note that if their interpretation of the radial velocity variations is correct, the radial velocities and the separation between the components should soon undergo very rapid variations. Vitrichenko (2002) analyzed the radial velocity of θ 1 Ori C, based on literature data and IUE spectra. From the temporal variations of the radial velocity he concluded that θ 1 Ori C is a close binary with a period of 66 days.…”

Section: Spectroscopic Results For the θ 1 Ori C Systemmentioning

confidence: 99%

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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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“…Finally, although the findings of Vitrichenko (2002) differ clearly from those of Donati et al (2002), our present data are unable to discriminate between them.…”

Section: Spectroscopic Results For the θ 1 Ori C Systemcontrasting

confidence: 51%

Section: Spectroscopic Results For the θ 1 Ori C Systemmentioning

confidence: 99%

Section: Spectroscopic Results For the θ 1 Ori C Systemmentioning

confidence: 99%

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Orbital motion of the massive multiple stars in the Orion Trapezium

Schertl

Balega

Preibisch

et al. 2003

A&A

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“…We used the spectra received by the IUE satellite (camera SWP, Folker 1994) as listed in Vitrichenko (2002), the data from Stahl et al (2008), the spectra from the Elodie Archive 1 , the spectra received by Stetsenko et al (2007) and kindly provided to us, and our newly obtained spectra as described in Table 1.…”

Section: Radial Velocitiesmentioning

confidence: 99%

“…The authors did not derive an orbital solution, however. Vitrichenko (2002) analyzed the RVs measured from the IUE spectra (Folker 1994) along with all available data from other observations. He concludes that Θ 1 Ori C is a triple system where three companions orbit its common center of mass.…”

Section: Introductionmentioning

confidence: 99%

Θ¹ Orionis C - A triple system?

Lehmann

Vitrichenko

Бычков

et al. 2010

A&A

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Context. As the brightest star in the Trapezium cluster, Θ 1 Ori C is the youngest and nearest to us among O-stars. It is considered to be a multiple system where the main component is an oblique magnetic rotator. Aims. Here, we aim at explaining the structure of the Θ 1 Ori C system. We check for a new hypothesis about the presence of a third component and try to derive the corresponding orbital solutions and the absolute masses of the components. Methods. We measured new radial velocities (RVs) of Θ 1 Ori C and and combined them with data from literature. For the analysis, we used multiple frequency search and iterative calculations of orbits based on the method of differential corrections, applying successive prewhitening to the data in both methods. Results are compared with those obtained from speckle observations. Results. We detected the impact of the known distant companion in the RVs of the primary and can now calculate a spectroscopic orbital solution that is consistent with the observed astrometric positions. We find evidence that Θ 1 Ori C is at least a triple system consisting of the primary, the known astrometric companion in a wide eccentric orbit with a period of 11 yr, and a second companion in a close eccentric orbit with a period of 61. d 5. We assign the additionally found period of 15. d 4 d to the rotation of the primary, which is in a 1:4 resonance with the close orbit. Derived masses are 31 M for the primary, 12 M for the distant, and 1 M for the close companion.

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

Kraus¹,

Weigelt²,

Balega

et al. 2009

A&A

108

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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A study of the radial velocity of the star Θ1 Ori C

Cited by 18 publications

References 12 publications

Orbital motion of the massive multiple stars in the Orion Trapezium

Orbital motion of the massive multiple stars in the Orion Trapezium

Θ¹ Orionis C - A triple system?

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

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A study of the radial velocity of the star Θ1 Ori C

Cited by 18 publications

References 12 publications

Orbital motion of the massive multiple stars in the Orion Trapezium

Orbital motion of the massive multiple stars in the Orion Trapezium

Θ1 Orionis C - A triple system?

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

Contact Info

Product

Resources

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Θ¹ Orionis C - A triple system?