The variable stellar wind of Rigel probed at high spatial and spectral resolution^{⋆,⋆⋆,⋆⋆⋆}

¹ Laboratoire Lagrange, UMR7293, Univ. Nice Sophia-Antipolis, CNRS, Observatoire de la Côte d’Azur, 06300 Nice, France
e-mail: Olivier.Chesneau@oca.eu
² European Southern Observatory, Alonso de Cordova 3107, Casilla 19001, 763-0355 Santiago, Chile
³ ZAH, Landessternwarte, Königstuhl 12, 69117 Heidelberg, Germany
⁴ Laboratoire d’Astrophysique de Marseille, Université de Provence, CNRS, 38 rue Frédéric Joliot-Curie, 13388 Marseille Cedex 13, France
⁵ Department of Physics & Astronomy, University College London, Gower Street, London, WC1E 6BT, UK
⁶ Instituto de Astronomía, Universidad Católica del Norte, Avenida Angamos 0610, Antofagasta, Chile
⁷ Astronomisches Institut, Ruhr-Universität Bochum, Universitätsstraße 150, 44801 Bochum, Germany

Received: 22 October 2013
Accepted: 1 May 2014

Abstract

Context. Luminous BA-type supergiants are the brightest stars in the visible that can be observed in distant galaxies and are potentially accurate distance indicators. The impact of the variability of the stellar winds on the distance determination remains poorly understood.

Aims. Our aim is to probe the inhomogeneous structures in the stellar wind using spectro-interferometric monitoring.

Methods. We present a spatially resolved, high-spectral resolution (R = 12 000) K-band temporal monitoring of the bright supergiant β Orionis (Rigel, B8 Iab) using AMBER at the Very Large Telescope Interferometer (VLTI). Rigel was observed in the Brγ line and its nearby continuum once per month over 3 months in 2006−2007, and 5 months in 2009−2010. These unprecedented observations were complemented by contemporaneous optical high-resolution spectroscopy. We analyse the near-IR spectra and visibilities with the 1D non-LTE radiative-transfer code CMFGEN. The differential and closure phase signals are evidence of asymmetries that are interpreted as perturbations of the wind.

Results. A systematic visibility decrease is observed across the Brγ line indicating that at a radius of about 1.25 R_∗ the photospheric absorption is filled by emission from the wind. During the 2006−2007 period the Brγ and likely the continuum forming regions were larger than in the 2009−2010 epoch. Using CMFGEN  we infer a mass-loss rate change of about 20% between the two epochs. We also find time variations in the differential visibilities and phases. The 2006−2007 period is characterised by noticeable variations in the differential visibilities in Doppler position and width and by weak variations in differential and closure phase. The 2009−2010 period is much quieter with virtually no detectable variations in the dispersed visibilities but a strong S-shaped signal is observed in differential phase coinciding with a strong ejection event discernible in the optical spectra. The differential phase signal that is sometimes detected is reminiscent of the signal computed from hydrodynamical models of corotating interaction regions. For some epochs the temporal evolution of the signal suggests the rotation of the circumstellar structures.