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Near-IR Observations of Vega-like Stars with the VLTI: β Pic, α PsA, ∊ Eri and τ Cet

Published online by Cambridge University Press:  26 May 2016

Emmanuel Di Folco ,
Pierre Kervella ,
Frédéric Thévenin ,
Pierre Morel ,
Armando Domiciano de Suza  and
Vincent Coudé du Foresto
Emmanuel Di Folco
Affiliation:
ESO, Karl Schwarzschild Str. 2, D-85748 Garching, Germany
Pierre Kervella
Affiliation:
ESO, Alonso de Cordova 3107, Casilla 19001, Santiago 19, Chile
Frédéric Thévenin
Affiliation:
Observatoire de la Cote d'Azur, BP 4229, F-06304 Nice, France
Pierre Morel
Affiliation:
Observatoire de la Cote d'Azur, BP 4229, F-06304 Nice, France
Armando Domiciano de Suza
Affiliation:
Observatoire de la CÔte d'Azur, Département Fresnel, CNRS UMR 6528, 2130 route de l'Observatoire, Caussols, F-06460 St Vellier de Thiey, France
Vincent Coudé du Foresto
Affiliation:
LESIA, FRE 2461, Observatoire de Paris-Meudon, 5 place J. Janssen, F-92190 Meudon, France

Abstract

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We have conducted K band interferometric observations of four nearby main-sequence Vega-like stars at the VLTI with very long baselines. The very high resolution allowed us to probe the innermost region of the disks, where planets are supposed to be formed. The diameters of three bright and nearby prototypes β Pictoris, Fomalhaut (α PsA) and ∊ Eridani as well as τ Ceti have been measured with VINCI, the VLTI commissioning instrument, with a high accuracy. The derived diameters were used to constrain their age with help of the evolution code CESAM. The precision achieved with VINCI allowed us to discuss the shape of their photosphere and the possible detection of warm circumstellar material within the narrow interferometric field of view.

Type
Part 2: Results from New Instrumentation
Information
Symposium - International Astronomical Union , Volume 219: Stars as Suns : Activity, Evolution and Planets , 2004 , pp. 75 - 79
Copyright
Copyright © Astronomical Society of the Pacific 2004 

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