The close-in companion of the fast rotating Be star Achernar

2008/04/22 by Pierre Kervella, P. Kervella, A. Domiciano de Souza +2
Mathematics · Physics and Astronomy · #Astronomy #Astronomy and Astrophysical Research #Astrophysics #Astrophysics and Star Formation Studies #Context (archaeology) #Emission spectrum #Geometry #History #Line (geometry) #Mathematics #Physics #Spectral line #Star (game theory) #Stars #Stellar, planetary, and galactic studies #Subgiant #astro-ph

paper · pdf · doi:10.1051/0004-6361:200809765

Accepted for publication as an A&A Letter. Astronomy and Astrophysics (2008) In press

arxiv created 2008/04/22 · openalex publication_date 2008/04/22 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05

Abstract

Context. The Be stars are massive dwarf or subgiant stars that present temporary emission lines in their spectrum, and particularly in the Hα line. The mechanism triggering these Be episodes is currently unknown, but binarity could play an important role.

Citations

• On the Determination of the Rotational Oblateness of Achernar
• JHKLM photometry - Standard systems, passbands, and intrinsic colors
• Spectroscopic observations of the δ Scorpii binary during its recent periastron passage
• The spinning-top Be star Achernar from VLTI-VINCI
• The interferometric diameter and internal structure of Sirius A
• The Two Micron All Sky Survey (2MASS)
• The environment of the fast rotating star Achernar