The fundamental parameters of the roAp star gamma Equulei

作者：Perraut K^*; Brandao I; Mourard D; Cunha M; Berio Ph; Bonneau D; Chesneau O; Clausse J M; Delaa O; Marcotto A; Roussel A; Spang A; Stee Ph; Tallon Bosc I; McAlister H; ten Brummelaar T; Sturmann J; Sturmann L; Turner N; Farrington C; Goldfinger P J

来源：Astronomy & Astrophysics, 2011, 526: A89.

DOI：10.1051/0004-6361/201015801

• methods: observational
• techniques: high angular resolution
• techniques: interferometric
• stars: individual: gamma Equ
• stars: fundamental parameters

Context. A precise comparison of the predicted and observed locations of stars in the H-R diagram is needed when testing stellar interior theoretical models. For doing this, one must rely on accurate, observed stellar fundamental parameters (mass, radius, luminosity, and abundances).
Aims. We determine the angular diameter of the rapidly oscillating Ap star, gamma Equ, and derive its fundamental parameters from this value.
Methods. We observed gamma Equ with the visible spectro-interferometer VEGA installed on the optical CHARA interferometric array, and derived both the uniform-disk angular diameter and the limb-darkened diameter from the calibrated squared visibility. We then determined the luminosity and the effective temperature of the star from the whole energy flux distribution, the parallax, and the angular diameter.
Results. We obtained a limb-darkened angular diameter of 0.564 +/- 0.017 mas and deduced a radius of R = 2.20 +/- 0.12 R-circle dot. Without considering the multiple nature of the system, we derived a bolometric flux of (3.12 +/- 0.21) x 10(-7) erg cm(-2) s(-1) and an effective temperature of 7364 +/- 235 K, which is below the previously determined effective temperature. Under the same conditions we found a luminosity of L = 12.8 +/- 1.4 L-circle dot. When the contribution of the closest companion to the bolometric flux is considered, we found that the effective temperature and luminosity of the primary star can reach similar to 100 K and similar to 0.8 L-circle dot lower than the values mentioned above.
Conclusions. For the first time, and thanks to the unique capabilities of VEGA, we managed to constrain the angular diameter of a star as small as 0.564 mas with an accuracy of about 3% and to derive its fundamental parameters. In particular the new values of the radius and effective temperature should bring further constraints on the asteroseismic modeling of the star.

• 出版日期2011-2