The binary system of the spinning-top Be star Achernar^⋆

¹ LESIA, Observatoire de Paris, Université PSL, CNRS, Sorbonne Université, Université Paris-Cité, 5 Place Jules Janssen, 92195 Meudon, France
e-mail: pierre.kervella@observatoiredeparis.psl.eu
² Université Côte-d’Azur, Observatoire de la Côte d’Azur, CNRS, Lagrange UMR 7293, CS 34229, 06304 Nice Cedex 4, France
³ European Southern Observatory, Karl-Schwarzschild-Str. 2, 85748 Garching, Germany
⁴ Universidad de Concepción, Departamento de Astronomía, Casilla 160-C, Concepción, Chile
⁵ Unidad Mixta Internacional Franco-Chilena de Astronomía (CNRS UMI 3386), Departamento de Astronomía, Universidad de Chile, Camino El Observatorio 1515, Las Condes, Santiago, Chile
⁶ European Southern Observatory, Alonso de Córdova 3107, Casilla, 19001 Santiago 19, Chile
⁷ Instituto de Astronomia, Geofísica e Ciéncias Atmosféricas, Universidade de São Paulo, Rua do Matão 1226, Cidade Universitária B-05508-900, São Paulo, SP, Brazil
⁸ National Radio Astronomy Observatory, 1003 Lopezville Road, Socorro, NM 87801, USA
⁹ Université Grenoble Alpes, CNRS, IPAG, 38000 Grenoble, France
¹⁰ Centrum Astronomiczne im. Mikołaja Kopernika, PAN, Bartycka 18, 00-716 Warsaw, Poland
¹¹ The CHARA Array of Georgia State University, Mount Wilson Observatory, Mount Wilson, CA 91023, USA

Received: 12 May 2022
Accepted: 24 August 2022

Abstract

Context. Achernar, the closest and brightest classical Be star, presents rotational flattening, gravity darkening, occasional emission lines due to a gaseous disk, and an extended polar wind. It is also a member of a close binary system with an early A-type dwarf companion.

Aims. We aim to determine the orbital parameters of the Achernar system and to estimate the physical properties of the components.

Methods. We monitored the relative position of Achernar B using a broad range of high angular resolution instruments of the VLT/VLTI (VISIR, NACO, SPHERE, AMBER, PIONIER, GRAVITY, and MATISSE) over a period of 13 years (2006−2019). These astrometric observations are complemented with a series of ≈750 optical spectra for the period from 2003 to 2016.

Results. We determine that Achernar B orbits the primary Be star on a seven-year period, eccentric orbit (e = 0.7258 ± 0.0015) which brings the two stars within 2 au at periastron. The mass of the Be star is found to be m_A = 6.0 ± 0.6 M_⊙ for a secondary mass of m_B = 2.0 ± 0.1 M_⊙ (the latter was estimated from modeling). We find a good agreement of the parameters of Achernar A with the evolutionary model of a critically rotating star of 6.4 M_⊙ at an age of 63 Ma. The equatorial plane of the Be star and the orbital plane of the companion exhibit a relative inclination of 30°. We also identify a resolved comoving low-mass star, which leads us to propose that Achernar is a member of the Tucana-Horologium moving group.

Conclusions. The proximity of Achernar makes this star a precious benchmark for stellar evolution models of fast rotators and intermediate mass binaries. Achernar A is presently in a short-lived phase of its evolution following the turn-off, during which its geometrical flattening ratio is the most extreme. Considering the orbital parameters, no significant interaction occurred between the two components, demonstrating that Be stars may form through a direct, single-star evolution path without mass transfer. Since component A will enter the instability strip in a few hundred thousand years, Achernar appears to be a promising progenitor of the Cepheid binary systems.