Interferometry, spectroscopy and astrometry of the bright eclipsing system Delta Velorum

Details Interferometry, spectroscopy and astrometry of the bright eclipsing system Delta Velorum Interferometry, spectroscopy and astrometry of the bright eclipsing system Delta Velorum

2012-03-12

arxiv.org/abs/1203.2653v1

Astronomy and Astrophysics

Astrophysics

Solar and Stellar Astrophysics

4 pages, 5 figures, in GREAT-ESF Workshop 'Orbital Couples: "Pas de Deux" in the Solar System and the Milky Way', Paris, IMCCE

Scientific paper

The bright southern star Delta Vel is a multiple system comprising at least three stars. Its brightest component, Delta Vel A, was identified in 2000 as one of the brightest eclipsing system in the sky. Its eclipses are easily observable with the unaided eye, a remarkable property shared only by Algol, Beta Aur, Alpha CrB and Psi Cen. We determined dynamical masses from a combination of spectroscopy, high-precision astrometry of the orbits of Aab-B and Aa-Ab using adaptive optics (VLT/NACO) and optical interferometry (VLTI/AMBER). The main eclipsing component is a pair of A-type stars in rapid rotation. We modeled the photometric and radial velocity measurements of the eclipsing pair Aa-Ab using a self consistent method based on physical parameters (mass, radius, luminosity, rotational velocity). From this modeling, we derive the fundamental parameters of the eclipsing stars with a typical accuracy of 1%. We find that they have similar masses, respectively 2.43 +/- 0.02 and 2.27 +/- 0.02 Msun. The physical parameters of the tertiary component (Delta Vel B) are also derived, although to a lower accuracy, as well as the parallax of the system, 39.8 +/- 0.4 mas. This value is in satisfactory agreement (-1.2 sigma) with the Hipparcos parallax of the system (pi_Hip =40.5 +/- 0.4 mas).

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