The nearby eclipsing stellar system δ Velorum - III. Self-consistent fundamental parameters and distance

@article{Mrand2011TheNE,
  title={The nearby eclipsing stellar system $\delta$ Velorum - III. Self-consistent fundamental parameters and distance},
  author={A. M{\'e}rand and Pierre Kervella and Theodor Pribulla and Monika G. Petr-Gotzens and Myriam Benisty and Antonella Natta and G. Duvert and Dieter Schertl and Martin Vannier},
  journal={Astronomy and Astrophysics},
  year={2011},
  volume={532}
}
The triple stellar system delta Vel (composed of two A-type and one F-type main sequence stars) is particularly interesting as it contains one of the nearest and brightest eclipsing binaries. It therefore presents a unique opportunity to determine independently the physical properties of the three components of the system, as well as its distance. We aim at determining the fundamental parameters (masses, radii, luminosities, rotational velocities) of the three components of delta Vel, as well… 

Interferometry, spectroscopy and high precision astrometry of δ Velorum

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2019 ) Tracking massive pairs

The analysis of eclipsing binaries with massive components enables to test stellar evolution models and track selected aspects of the structure of early-type stars. Stellar pairs with B-type

Tracking massive pairs

The analysis of eclipsing binaries with massive components enables to test stellar evolution models and track selected aspects of the structure of early-type stars. Stellar pairs with B-type

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Binaries and Multiple Systems Observed with the CHARA, NPOI, SUSI and VLTI Interferometric Eyes

  • P. Stee
  • Physics
    Proceedings of the International Astronomical Union
  • 2011
Abstract In this review I will present recent results between 2007 and 2011 based on interferometric observations of binaries and multiple systems with the VLTI, NPOI, SUSI and CHARA instruments. I

References

SHOWING 1-10 OF 35 REFERENCES

Interferometric observations of the multiple stellar system δ Velorum

Context. The nearby (∼24 pc) triple stellar system δ Velorum contains a close, eclipsing binary (Aa, Ab) discovered in 2000. Multiple systems provide an opportunity to determine the set of

The nearby eclipsing stellar system δ Velorum

Context. The stellar system δVel contains the brightest eclipsing binary in the southern sky (δVel A), and a nearby third star located ≈0.6′′ away (δVel B). The proximity of δVel B (usable as a

The nearby eclipsing stellar system $\delta$ Velorum - I. Origin of the infrared excess from VISIR and NACO imaging

Context. The triple stellar system δ Vel system presents a significant infrared excess, whose ori gin is still being debated. A large infrared bow shock has been discovered using Spitzer/MIPS

Radial velocities of HIPPARCOS southern B8-F2 type stars

Radial velocities have been determined for a sample of B8-F2 type stars observed by the Hipparcos satellite. Observations were obtained within the frame- work of an ESO key-program. Radial velocities

Astrometric and photometric monitoring of GQ Lupi and its sub-stellar companion

Context. Neuhauser et al. (2005, A&A, 435, L13) presented direct imaging evidence for a sub-stellar companion to the young T Tauri star GQ Lupi. Common proper motion was highly significant, but no

Cepheid distances from infrared long-baseline interferometry III. Calibration of the surface brightness-color relations

The recent VINCI/VLTI observations presented in Paper I have nearly doubled the total number of available angular diameter measurements of Cepheids. Taking advantage of the significantly larger color

IRAS OBSERVATIONS OF MATTER AROUND NEARBY STARS.

A systematic search of the IRAS point-source catalog has identified eight new nearby stars which are "Vega-like" in terms of their large 60-micron excess. This brings to twelve, of the set of 36

Circumstellar material in the Vega inner system revealed by CHARA/FLUOR

Context. Only a handful of debris disks have been imaged up to now. Due to the need for high dynamic range and high angular resolution, very little is known about the inner planetary region, where

First Results from the CHARA Array. VII. Long-Baseline Interferometric Measurements of Vega Consistent with a Pole-On, Rapidly Rotating Star

We have obtained high-precision interferometric measurements of Vega with the CHARA Array and FLUOR beam combiner in the K′ band at projected baselines between 103 and 273 m. The measured visibility

CCD Speckle Observations of Binary Stars from the Southern Hemisphere. II. Measures from the Lowell-Tololo Telescope during 1999

Speckle observations of 145 double stars and suspected double stars are presented and discussed. On the basis of multiple observations, a total of 280 position angle and separation measures are