The Fast Rotating Star 51 Oph Probed by VEGA/CHARA

N. Jamialahmadi; P. Berio; A. Meilland; K. Perraut; D. Mourard; B. Lopez; P. Stee; N. Nardetto; B. Pichon; J.M. Clausse; A. Spang; H. McAlister; T. ten Brummelaar

doi:10.1051/eas/1571077

All issues

Volume 71-72 (2015)

EAS Publications Series, 71-72 (2015) 327-329

Abstract

Issue		EAS Publications Series Volume 71-72, 2015 The Physics of Evolved Stars: A Conference Dedicated to the Memory of Olivier Chesneau


Page(s)		327 - 329
Section		Modeling, Evolution
DOI		https://doi.org/10.1051/eas/1571077
Published online		01 December 2015

The Physics of Evolved Stars: A Conference Dedicated to the Memory of Olivier Chesneau
E. Lagadec, F. Millour and T. Lanz (eds)
EAS Publications Series, 71–72 (2015) 327-329

The Fast Rotating Star 51 Oph Probed by VEGA/CHARA

N. Jamialahmadi¹, P. Berio², A. Meilland², K. Perraut³, D. Mourard², B. Lopez², P. Stee², N. Nardetto², B. Pichon², J.M. Clausse², A. Spang², H. McAlister⁴ and T. ten Brummelaar¹^,2

¹ European Southern Observatory, Karl-Schwarzschild-Str. 2, 85748 Garching, Munich, Germany
² Laboratoire Lagrange, UMR 7293, Univ. Nice Sophia-Antipolis, CNRS, Observatoire de la Côte d*Azur, 06304 Nice, France
³ Institut d*Astrophysique et de Planétologie de Grenoble, CNRS-UJF UMR 5571, 414 rue de la Piscine, 38400 St-Martin d*Hères, France
⁴ CHARA Array, Mount Wilson Observatory, 91023 Mount Wilson CA, USA

e-mail: njamiala@eso.eu

Abstract

Stellar rotation is a key in our understanding of both mass-loss and evolution of intermediate and massive stars. It can lead to anisotropic mass-loss in the form of radiative wind or an excretion disk. We used the VEGA visible beam combiner installed on the CHARA array that reaches a sub milliarcsecond resolution. We derived, for the first time, the extension and flattening of 51 Oph photosphere. We found an elongated ratio of 1.45 ± 0.12.