Orbits for five southern visual binaries

Argyle, R. W.; Alzner, A.; Horch, Elliott

doi:10.1051/0004-6361:20011805

Cited by 18 publications

(17 citation statements)

References 16 publications

(10 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The total mass of the whole triple system δ Velorum as determined by Argyle et al (2002) Fig. 2), confirming the orbit of Argyle et al (2002).…”

Section: The Triple System δ Velorumsupporting

confidence: 68%

“…= −0.15 (Popper 1980), we derive the absolute visual magnitudes of the components to be M V (Aa) = +0.519 and M V (Ab) = +0.719. This gives a combined magnitude of M V (A) = −0.138, which is substantially brighter than the reliable value determined from the observed visual brightness and Hipparcos distance by Argyle et al (2002). This simple computation, however, does not take into account that the observer faces the coldest (equatorial) part of the system.…”

Section: The Triple System δ Velorummentioning

confidence: 67%

“…The expected semi-amplitude, for the visual orbit of Argyle et al (2002), is about 1.5 h. In view of the large v sin i of the components and the blending of their profiles, systemic-velocity changes in the eclipsing pair would be hardly detectable nor useful. …”

Section: Discussion and Future Workmentioning

confidence: 96%

“…For a long time, it has been known that it is a visual binary composed of the brighter component A with H P = 1.99 and the fainter component B with H P = 5.57 orbiting in a wide 142-year orbit (see Argyle et al 2002).…”

Section: Introductionmentioning

confidence: 99%

See 3 more Smart Citations

The nearby eclipsing stellar systemδVelorum

Pribulla¹,

Mérand²,

Kervella³

et al. 2011

A&A

View full text Add to dashboard Cite

Context. The nearby multiple system δ Velorum contains a widely detached eclipsing binary and a third component. Aims. We take advantage of this system offering the opportunity to determine the set of fundamental parameters (masses, luminosities, and radii) of three coeval stars with sufficient precision to test models of stellar evolution. Methods. Extensive high-resolution spectroscopy is analyzed by the broadening function technique to provide the first spectroscopic orbit of the eclipsing pair. Simultaneous analysis of the spectroscopic data and the SMEI satellite light curve is performed to provide astrophysical parameters for the components. We use a modified Roche model assuming an eccentric orbit and asynchronous rotation. Results. The observations show that components of the eclipsing pair rotate at about two-thirds of the break-up velocity, which excludes any chemical peculiarity and results in a non-uniform surface brightness. Although the inner orbit is eccentric, no apsidal motion is seen during the SMEI photometric observations. For the inner orbit, the orbital parameters are eccentricity e = 0.290, longitude of the periastron passage ω = 109 • , and inclination 89.0 • . Conclusions. The component masses of M Aa = 2.53 ± 0.11 M , M Ab = 2.37 ± 0.10 M , and M B ∼ 1.5 M combined with the inferred radii of the Aa and Ab components indicate that the eclipsing pair has already left the main sequence and that the estimated age of the system is about 400 Myr.

show abstract

“…The total mass of the whole triple system δ Velorum as determined by Argyle et al (2002) Fig. 2), confirming the orbit of Argyle et al (2002).…”

Section: The Triple System δ Velorumsupporting

confidence: 68%

Section: The Triple System δ Velorummentioning

confidence: 67%

Section: Discussion and Future Workmentioning

confidence: 96%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

The nearby eclipsing stellar systemδVelorum

Pribulla¹,

Mérand²,

Kervella³

et al. 2011

A&A

View full text Add to dashboard Cite

show abstract

“…A preliminary orbit was given by Argyle et al (2002), but since then periastron passage has occurred (completely unobserved) and the companion has moved a further 140 degrees. Recent observations (Table 4) have allowed a new orbit to be calculated by AA which gives much smaller uncertainties in the orbital elements.…”

Section: Beta Phe -Wds 01061-4643mentioning

confidence: 99%

Micrometric measures and orbits of southern visual double stars

Argyle

Alyner²,

Leeuwen

2015

Astron Nachr

Self Cite

View full text Add to dashboard Cite

show abstract

Relative astrometry and near‐infrared differential photometry of nearby southern orbital binaries with adaptive optics

et al. 2013

View full text Add to dashboard Cite

We present relative astrometry and differential photometry measurements for a sample of nearby southern orbital binaries making use of the technique of Adaptive Optics. The observations were made in December 2000, with the ADONIS camera mounted at the 3.6-m ESO telescope from La Silla Observatory, equipped with the broad-band near-infrared filters (J-, H-, K-passbands). Our sample contains stars which do not fit very well the empirical mean mass-luminosity relation (according to our previous study), but for which accurate parallaxes (determined by the Hipparcos satellite) and highquality orbits were available thanks to many previous efforts. We derived accurate positions and J, H, K magnitudes of the individual components of those binaries. The individual stellar components have near-infrared colour indices well grouped in those plots and are comparable to standard single stars. The data reduction procedure used for deriving those results is described in detail. It is based on a least-squares fit of Moffat-Lorentz profiles in direct imaging for well-resolved systems and on Fourier analysis for very close pairs.

show abstract

Orbits for five southern visual binaries

Abstract: (2000), has an unexpectedly short period.

Cited by 18 publications

References 16 publications

The nearby eclipsing stellar systemδVelorum

The nearby eclipsing stellar systemδVelorum

Micrometric measures and orbits of southern visual double stars

Relative astrometry and near‐infrared differential photometry of nearby southern orbital binaries with adaptive optics

Contact Info

Product

Resources

About