A realistic twodimensional model of Altair
Abstract
Context. Fast rotation is responsible for important changes in the structure and evolution of stars and the way we see them. Optical long baseline interferometry now allows for the study of its effects on the stellar surface, mainly gravity darkening and flattening.
Aims: We aim to determine the fundamental parameters of the fastrotating star Altair, in particular its evolutionary stage (represented here by the core hydrogen mass fraction X_{c}), mass, and differential rotation, using stateoftheart stellar interior and atmosphere models together with interferometric (ESOVLTI), spectroscopic, and asteroseismic observations.
Methods: We use ESTER twodimensional stellar models to produce the relevant surface parameters needed to create intensity maps from atmosphere models. Interferometric and spectroscopic observables are computed from these intensity maps and several stellar parameters are then adjusted using the publicly available MCMC algorithm Emcee.
Results: We determined Altair's equatorial radius to be R_{eq} = 2.008 ± 0.006 R_{⊙}, the position angle PA = 301.1 ± 0.3°, the inclination i = 50.7 ± 1.2°, and the equatorial angular velocity Ω = 0.74 ± 0.01 times the Keplerian angular velocity at equator. This angular velocity leads to a flattening of ɛ = 0.220 ± 0.003. We also deduce from the spectroscopically derived v sin i ≃ 243 km s^{1}, a true equatorial velocity of ∼314 km s^{1} corresponding to a rotation period of 7h46m (∼3 cycles/day). The data also impose a strong correlation between mass, metallicity, hydrogen abundance, and core evolution. Thanks to asteroseismic data, and provided our frequencies identification is correct, we constrain the mass of Altair to 1.86 ± 0.03 M_{⊙} and further deduce its metallicity Z = 0.019 and its core hydrogen mass fraction X_{c} = 0.71, assuming an initial solar hydrogen mass fraction X = 0.739. These values suggest that Altair is a young star ∼100 Myr old. Finally, the 2D ESTER model also gives the internal differential rotation of Altair, showing that its core rotates approximately 50% faster than the envelope, while the surface differential rotation does not exceed 6%.
Based on VLTI observations performed at ESO, Chile under programme IDs 60.A9164(A), 87.D0150(A), and 094.C0232(A).
 Publication:

Astronomy and Astrophysics
 Pub Date:
 January 2020
 DOI:
 10.1051/00046361/201936830
 arXiv:
 arXiv:1912.03138
 Bibcode:
 2020A&A...633A..78B
 Keywords:

 stars: individual: Altair;
 stars: interiors;
 stars: atmospheres;
 stars: rotation;
 stars: fundamental parameters;
 stars: oscillations;
 Astrophysics  Solar and Stellar Astrophysics
 EPrint:
 20 pages, 20 figures, accepted for publication in A&