DEFRÈRE, D.; ABSIL, O.; AUGEREAU, J. C.; DI FOLCO, E.; COUDÉ DU FORESTO, V.; LE BOUQUIN, J. B.; MÉRAND, A.; MOLLIER, B.

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DEFRÈRE, D.

ABSIL, O.
Université de Liège

AUGEREAU, J. C.
Institut de Planétologie et d'Astrophysique de Grenoble [IPAG ]

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Ce document a été publié dans

EPSC-DPS Joint Meeting 2011, held 2-7 October 2011 in Nantes, France, p.1084, 2011, EPSC-DPS Joint Meeting 2011, held 2-7 October 2011 in Nantes, France, p.1084, 2011, EPSC-DPS Joint Meeting 2011, 2011, Nantes. 2011-10p. 1084

Résumé en anglais

Most debris disks resolved so far show extended structures located at tens to hundreds AU from the host star, and are more analogous to our solar system's dusty Kuiper belt than to the AU-scale zodiacal disk inside our solar system's asteroid belt. Over the last few years however, a few hot debris disks have been detected around a handful of main sequence stars thanks to the advance of infrared interferometry. The grain populations derived from these observations are quite intriguing, as they point towards very high dust replenishment rates, high cometary activity or major collisional events. In this talk, we review the ongoing efforts to detect bright exozodiacal disks with precision near-infrared interferometry in both hemispheres with CHARA/FLUOR and VLTI/PIONIER. We discuss preliminary statistical trends on the occurrence of bright exozodi around nearby main sequence stars and show how this information could be used to constrain the global architecture and evolution of debris disks.< Réduire

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Unités de recherche

Laboratoire d'Astrophysique de Bordeaux (LAB) - UMR 5804