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VINCI/VLTI Observations of Main Sequence Stars

Published online by Cambridge University Press:  26 May 2016

Pierre Kervella ,
Frédéric Thévenin ,
Pierre Morel ,
Janine Provost ,
Gabrielle Berthomieu ,
Damien Ségransan ,
Didier Queloz ,
Pascal Bordé ,
Emmanuel Di Folco  and
Thierry Forveille
Pierre Kervella
Affiliation:
ESO, Alonso de Cordova 3107, Casilla 19001, Santiago 19, Chile
Frédéric Thévenin
Affiliation:
Observatoire de la CÔte d'Azur, BP 4229, F-06304 Nice, France
Pierre Morel
Affiliation:
Observatoire de la CÔte d'Azur, BP 4229, F-06304 Nice, France
Janine Provost
Affiliation:
Observatoire de la CÔte d'Azur, BP 4229, F-06304 Nice, France
Gabrielle Berthomieu
Affiliation:
Observatoire de la CÔte d'Azur, BP 4229, F-06304 Nice, France
Damien Ségransan
Affiliation:
Observatoire de Genève, CH-1290 Sauverny, Switzerland
Didier Queloz
Affiliation:
Observatoire de Genève, CH-1290 Sauverny, Switzerland
Pascal Bordé
Affiliation:
Observatoire de Paris, 5, pl. Jules Janssen, F-92195 Meudon, France
Emmanuel Di Folco
Affiliation:
ESO, Karl-Schwarzschild-Str. 2, D-95748 Garching, Germany
Thierry Forveille
Affiliation:
CFHT Corporation, PO Box 1597, Kamuela, HI 96743, USA

Abstract

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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.

Type
Part 2: Results from New Instrumentation
Information
Symposium - International Astronomical Union , Volume 219: Stars as Suns : Activity, Evolution and Planets , 2004 , pp. 80 - 84
Copyright
Copyright © Astronomical Society of the Pacific 2004 

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