The spinning-top Be star Achernar from VLTI-VINCI

• Published in: Astronomy and astrophysics (Berlin) 2003-09, Vol.407 (3), p.L47-L50
• Main Authors: A. Domiciano de Souza, Kervella, P., Jankov, S., Abe, L., Vakili, F., di Folco, E., Paresce, F.
• Format: Article
• Language: English
• Subjects: Astrophysics; Sciences of the Universe; stars: emission-line; stars: individual: Achernar; stars: rotation; techniques: high angular resolution; techniques: interferometric
• ISSN: 0004-6361; 1432-0746; 1432-0756
• DOI: 10.1051/0004-6361:20030786

We report here the first observations of a rapidly rotating Be star, α Eridani, using Earth-rotation synthesis on the Very Large Telescope (VLT) Interferometer. Our measures correspond to a $2a/2b = 1.56\pm0.05$ apparent oblate star, $2a$ and $2b$ being the equivalent uniform disc angular diameters in the equatorial and polar direction. Considering the presence of a circumstellar envelope (CSE) we argue that our measurement corresponds to a truly distorted star since α Eridani exhibited negligible Hα emission during the interferometric observations. In this framework we conclude that the commonly adopted Roche approximation (uniform rotation and centrally condensed mass) should not apply to α Eridani. This result opens new perspectives to basic astrophysical problems, such as rotationally enhanced mass loss and internal angular momentum distribution. In addition to its intimate relation with magnetism and pulsation, rapid rotation thus provides a key to the Be phenomenon: one of the outstanding non-resolved problems in stellar physics.