VINCI, the VLTI commissioning instrument: status after one year of operations at Paranal

Kervella, P.; Gitton, Philippe B.; Ségransan, D.; Folco, E. Di; Kern, P.; Kiekebusch, M.; Duc, Than Phan; Longinotti, Antonio; Foresto, V. Coudé du; Ballester, P.; Sabet, Cyrus; Cotton, W. D.; Schoeller, Markus; Wilhelm, Rainer

doi:10.1117/12.459345

Cited by 44 publications

(16 citation statements)

References 9 publications

(9 reference statements)

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“…Dedicated observations of Achernar have been carried out during the ESO period 70, from 11 September to 12 November 2002, with quasi-uniform time coverage, on the VLT Interferometer (VLTI, Glindemann et al 2003) equipped with the VINCI beam combiner (Kervella et al 2003a). This instrument recombines the light from two telescopes in the astronomical K band, which is centered at 2.2 µm and covers 0.4 µm.…”

Section: Observations and Data Processingmentioning

confidence: 99%

The spinning-top Be star Achernar from VLTI-VINCI

Souza¹,

Kervella²,

Jankov³

et al. 2003

A&A

217

170

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Abstract. We report here the first observations of a rapidly rotating Be star, α Eridani, using Earth-rotation synthesis on the Very Large Telescope (VLT) Interferometer. Our measures correspond to a 2a/2b = 1.56 ± 0.05 apparent oblate star, 2a and 2b being the equivalent uniform disc angular diameters in the equatorial and polar direction. Considering the presence of a circumstellar envelope (CSE) we argue that our measurement corresponds to a truly distorted star since α Eridani exhibited negligible Hα emission during the interferometric observations. In this framework we conclude that the commonly adopted Roche approximation (uniform rotation and centrally condensed mass) should not apply to α Eridani. This result opens new perspectives to basic astrophysical problems, such as rotationally enhanced mass loss and internal angular momentum distribution. In addition to its intimate relation with magnetism and pulsation, rapid rotation thus provides a key to the Be phenomenon: one of the outstanding non-resolved problems in stellar physics.

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Section: Observations and Data Processingmentioning

confidence: 99%

The spinning-top Be star Achernar from VLTI-VINCI

Souza¹,

Kervella²,

Jankov³

et al. 2003

A&A

217

170

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“…Because numerous new studies and observational constraints (like the direct diameter) exist today, we re-examined the status of Procyon. Our models were constrained using the spectroscopic effective temperature and the linear diameter value that we derived from our observations with the VINCI/VLTI instrument (Kervella et al 2000;2003a). Figure 2 (left) shows the evolutionary tracks of three models that converge into the uncertainty box in the HR diagram.…”

Section: Procyon A: the Synergy Of Interferometry And Asteroseismologymentioning

confidence: 99%

Stellar radii from long-baseline interferometry

Kervella¹

2008

Proc. IAU

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Abstract. Long baseline interferometers now measure the angular diameters of nearby stars with sub-percent accuracy. They can be translated in photospheric radii when the parallax is known, thus creating a novel and powerful constraint for stellar models. I present applications of interferometric radius measurements to the modeling of main sequence stars. Over the last few years, we obtained accurate measurements of the linear radius of many of the nearest stars: Procyon A, 61 Cyg A & B, α Cen A & B, Sirius A, Proxima... Firstly, I describe the example of our modeling of Procyon A (F5IV-V) with the CESAM code, constrained using spectrophotometry, the linear radius, and asteroseismic frequencies. I also present our recent results on the low-mass 61 Cyg system (K5V+K7V), for which asteroseismic frequencies have not been detected yet.

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“…Thanks to high precision inter-2 P. Kervella et al ferometric measurements with the VLTI , equipped with the VINCI beam combiner (Kervella et al 2000;Kervella et al 2003a), we are in the process of producing a coherent list of angular diameters of nearby MS stars. The goal of our program is to refine our knowledge of their basic properties: age, metallicity, helium content, etc...…”

Section: Scientific Rationalementioning

confidence: 99%

VINCI/VLTI Observations of Main Sequence Stars

Kervella

Thévenin

Morel

et al. 2004

Symp. - Int. Astron. Union

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Abstract. Main Sequence (MS) stars are by far the most numerous class in the Universe. They are often somewhat neglected as they are relatively quiet objects (but exceptions exist), though they bear testimony of the past and future of our Sun. An important characteristic of the MS stars, particularly the solar-type ones, is that they host the large majority of the known extrasolar planets. Moreover, at the bottom of the MS, the red M dwarfs pave the way to understanding the physics of brown dwarfs and giant planets. We have measured very precise angular diameters from recent VINCI/VLTI interferometric observations of a number of MS stars in the K band, with spectral types between A1V and M5.5V. They already cover a wide range of effective temperatures and radii. Combined with precise Hipparcos parallaxes, photometry, spectroscopy as well as the asteroseismic information available for some of these stars, the angular diameters put strong constraints on the detailed models of these stars, and therefore on the physical processes at play.

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VINCI, the VLTI commissioning instrument: status after one year of operations at Paranal

Cited by 44 publications

References 9 publications

The spinning-top Be star Achernar from VLTI-VINCI

The spinning-top Be star Achernar from VLTI-VINCI

Stellar radii from long-baseline interferometry

VINCI/VLTI Observations of Main Sequence Stars

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